text:
\section{Introduction}
Recent years have seen dramatic progress in studies of the early universe, in large part due to sensitive observations with the Wide Field Camera 3 (WFC3) on {\em HST} which detects
the rest-frame UV light of distant galaxies. Studies now routinely identify large numbers of Lyman Break Galaxies (LBGs) in the first billion years of the universe (redshifts $6<z<8$) at the edge of the reionization epoch (e.g., Oesch et al. 2012; McLure et al. 2013; Finkelstein et al. 2012; Grazian et al. 2012, Schmidt et al. 14). Recently, Hubble pushed the frontier even further, finding several galaxies at higher redshifts $z>9$ (around 500 million years after the Big Bang, e.g., Bouwens et al. 2011, Zheng et al. 2012, Ellis et al. 2013, Oesch et al. 2014).

While HST is crucial for selecting the galaxies and determining the redshifts, {\em Spitzer}/IRAC (IRAC; Fazio et al. 2004) excels at detecting the infrared emission of high redshift galaxies. IRAC is currently the only instrument capable of measuring the rest-frame optical light of sources at $4 < z < 10$. The combination of Hubble and Spitzer has proven extremely powerful and provided estimates of the build up of the stellar mass density (e.g., Labb\'e et al. 2010, Gonzalez et al. 2011, Stark et al. 2013, Oesch et al. 2014, \citealt{Duncan14,Grazian14}) and the average specific SFR at $3 < z < 7$ (Gonzalez et al. 2010,2014, Stark et al. 2013, \citealt{Steinhardt14,Salmon14}). Comparing average IRAC colors of redshift $z\sim4-8$ galaxies subsequently showed that star forming galaxies must exhibit very strong nebular emission lines, boosting the Spitzer/IRAC photometry (e.g., \citealt{Sch10}, Labb\'e et al. 2010a,2010b,2013, Shim et al. 2011, Stark et al. 2013, Gonzalez et al. 2014, Smit et al. 2014). This realization has led to the first estimates of nebular emission line equivalent width at $z>4$ and improved estimates of the stellar masses (e.g., Shim et al. 2011, Labb\'e et al. 2013, Stark et al. 2013), which is of vital importance for understanding the mass build up, feedback,  and metal production in the earliest stages of galaxy formation. The current-best example of joint Hubble+Spitzer studies was the robust detection of a small sample of very bright $z\sim10$ candidate galaxies and a first estimate of the galaxy stellar mass density at only 500 Myr after the Big Bang (Oesch et al. 2014). The joint {\it HST}+{\it Spitzer} Frontier Fields campaigns provided other examples of bright, lensed high redshift galaxies (e.g., \citealt{Atek14,Laporte14,Zheng14,Bradac14})

\figlayout

Nevertheless, Spitzer/IRAC observations of earlier programs such as
GOODS (PID 194; PI Dickinson) were only deep enough to individually
detect a small fraction of the $z>6$ sources. For example, Labb\'e et
al. 2010b reported only 2/13 detected at $>5\sigma$ from a sample of
$H_{AB}<27.5$ galaxies at $z\sim7$ over the HUDF. Stacking was necessary to access typical $<L^*$ galaxies (e.g., Labb\'e et al. 2010a) as the $3.6\mu m-4.5\mu m$\ fluxes of individual sources were too low signal-to-noise (SNR) to be useful. In general, to extract meaningful information from the rest-frame optical SEDs, it is necessary to obtain SNR ratios of $>5$ in each of the $3.6$ and $4.5\mu$m band for typical sources at $z>7$.

\begin{deluxetable*}{lllcrrrr}
\leavevmode
\tablecaption{Summary of IRAC observations}
\tablecolumns{5}
\tablehead{
\colhead{program} & \colhead{PID} & \colhead{PI} & \colhead{max exp.(h)$^a$} & $\#$ pointings & \colhead{total exp.(h)} & \colhead{$\#$ frames} & SSC pipeline version$^d$}
\startdata \\
IUDF      & 70145  & Labb\'e   & 100 & 3 & 215.3   &  8280  & S19.0.0/S18.18.0 \\ \\
IGOODS    &  10076 & Oesch     & 46  & 2 & 65.5    &  2520 &  S19.1.0 \\ \\
GOODS     &  194$^c$   & Dickinson & 46  & 8 & 180.4   &  3356  & S18.25.0 \\ \\
ERS       & 70204 & Fazio      & 75  & 2 & 162.9  &  6264   &  S18.18.0\\ \\
S-CANDELS & 80217  & Fazio     & 25  & 4 & 101.1  & 3888   & S19.0.0/S19.1.0 \\ \\
SEDS      & 60022  & Fazio     & 12  & 20$^b$ & 209.3$^b$ &  8051  & S19.0.0/S18.18.0 \\ \\
UDF2      & 30866$^c$  & Bouwens   & 28.1 & 1 & 28.1 &  1080   & S18.25.0  \\ \\
\tableline \\
total & & & & & 962.6 & 33439  & \\
\add{\tablenotetext{a}{Maximum exposure time per position on the sky per channel.}}
\tablenotetext{b}{Only the central $\sim60$\% of the full SEDS data are used.}
\tablenotetext{c}{Cryogenic mission observations; all other programs are warm mission.}
\tablecomments{Program PID 20708 was omitted because the exposure time is negligible over
the central parts of the GOODS-S region.}
\tablenotetext{d}{The calibration pipelines used were the most recent available from the Spitzer
heritage archive at the time of writing. No significant changes since S18.18.0 have
been reported for 3.6 and 4.5\micron\ observations.}
\label{tab:observations}
\end{deluxetable*}

\begin{deluxetable}{lllcc}
\leavevmode
\tablecaption{Summary of individual AORs}
\tablecolumns{5}
\tablewidth{8cm}
\tablehead{
\colhead{PID} & \colhead{AOR key} & \colhead{MJD$^a$} & \colhead{area$_{50}^b$} & \colhead{$<$exptime$>_{50}^c$}  }
\startdata \\
       70145  &  40849920 & 55487.9259899 &   41.5 &  1.41 \\
       70145  &  40850176 & 55493.6466019 &   36.5 &  1.55 \\
       70145  &  40850432 & 55493.5162173 &   36.1 &  1.57 \\
       70145  &  40850688 & 55611.5557390 &   34.4 &  1.61 \\
       70145  &  40850944 & 55603.7885426 &   36.5 &  1.56 \\
\tablenotetext{a}{Modified Julian Day (JD-2400000.5) in UTC at start of observation}
\tablenotetext{b}{Total area in arcmin$^2$ with $>50\%$ of the maximum exposure time on sky.}
\tablenotetext{c}{Mean exposure time in hour over area$_{50}$.}
\tablecomments{Table 2 is published in its entirety in the electronic edition of ApJS. A portion is shown here for guidance regarding its form and content.}
\label{tab:aor}
\end{deluxetable}

To achieve this we initiated two ultradeep surveys in areas with existing ultradeep ACS+WFC3 data. The first was the cycle 7 IRAC Ultradeep Field (IUDF) program (PI Labb\'e; PID 70145) covering the HUDF/XDF and the two HUDF parallels to $\sim50-100$ hours. The second was the IRAC Legacy over GOODS (IGOODS) program in cycle 10 (PI Oesch; PID 10076), which was aimed at filling out half of the GOODS-South and GOODS-North areas to $\sim200$ hours depth, but which was only $10\%$ completed before being terminated.

This paper described the survey design, data reduction, image quality analysis, and presents the public data release of the IUDF and IGOODS programs, after combining the two ultradeep programs with all archival data over GOODS-South. The paper is structured as follows: \S2 describes the observations, section \S3 summarizes the data reduction and introduces a new technique for creating PSF maps, \S4 describes the resulting ultradeep IRAC mosaics, their properties, and simulations to test prior-based photometry, \S5 discusses the role of IRAC photometry for high redshift galaxies, while a summary is provided in \S6. \ \\

\section{Observations}

The IRAC surveys were all conducted in a single area of the sky, approximately centered on the HUDF in the GOODS-South field around $\alpha = 03:33,\ \delta=-27:48$. This field is
very well suited for IRAC surveys as it has low infrared background and excellent visibility for Spitzer. GOODS-South and the HUDF enjoy the highest quality optical+NIR observations from Hubble (e.g., Giavalisco et al. 2004, Beckwith et al. 2006, Grogin et al. 2011, Koekemoer et al. 2011, Illingworth et al. 2013, Ellis et al. 2013). The high resolution imaging data at shorter wavelengths are necessary for detecting high redshift galaxies and determining their redshift from the location of the redshifted Lyman break. These HUDF data have resulted in some of the largest known samples of high-redshift $z>7$ galaxies. As we shall see, the knowledge of the prior position and size of all sources in the field enables accurate modeling and extraction of the IRAC fluxes.

The GOODS-South field enables the maximum efficiency of any IRAC survey. The existing contiguous WFC3+ACS mosaic over scales of $10-15$ arcmin fills the full IRAC footprint. It also enables parallel $3.6\mu m$\ and $4.5\mu m$\ observations, which is relevant as high redshift studies require equally deep observations in both IRAC bands. Finally, very substantial investments in IRAC imaging have already been made in the GOODS fields (amounting to $\gtrsim 500 $ hour per band) so it is
more efficient to continue to build upon previous programs rather than starting from scratch.

Here we combine all programs to create single, contiguous ultra-deep images in the $3.6\mu m$\ and $4.5\mu m$\ bands. Below we discuss the individual programs that contributed to the data that were used
to construct the field (dubbed "IRAC Ultra Deep Field", IUDF). \\

\subsection{IRAC Ultradeep Field (IUDF)}
The IUDF cycle 7 program integrated for 210 hours in both IRAC filters, covering the HUDF/XDF
WFC3 field of the HUDF09 survey (PI Illingworth), including its two flanking fields HUDF09-1 and HUDF09-2. These fields are unique due to the concentrated investment of HST time and the large existing samples of $\sim$190 $z>7$ galaxies available immediately for study (Bouwens et al. 2014).

While the HUDF was previously covered with IRAC with 46 hours of cryogenic observations from GOODS (PI Dickinson), the parallel HUDF1 and HUDF2 had received limited and uneven coverage. The IUDF solves this by observing both HUDF parallels to $50-100$ hour at $3.6\mu m$\ and $4.5\mu m$, while using
roll angle constraints to obtain deeper imaging on the HUDF/XDF, increasing the exposure time to $100-120$ hour at $3.6\mu m$\ and $4.5\mu m$. The HUDF + parallels are the deepest-ever ACS+WFC3+IRAC of any field on the sky. \\

\subsection{IRAC Legacy over GOODS (IGOODS)}

The completion of the IUDF and the success of the first joint ultradeep WFC3+IRAC analyses in the HUDF/XDF (e.g., Oesch et al. 2012,2013, Labb\'e et al. 2013) demonstrated the scientific value of deep IRAC data as well as the feasibility of ultradeep studies. However, much larger samples to even deeper limits are needed for a proper characterization of the $z>7$ universe.

The IGOODS cycle 10 aimed to achieve this by increasing the IRAC depth to a homogenous 200 hours per sky position, while covering much larger areas $\sim 200$ arcmin$^2$ in GOODS-South and GOODS-North. These depths and areas are a sweet spot:  sensitive enough to provide direct detections of sub-L* star forming galaxies at $z\sim8$, while providing enough area for large samples and good statistics ($>200$ galaxies at $z>7$ with $>5\sigma$ IRAC photometry).

Of the approved 800 hours, 200 were earmarked as higher priority to demonstrate the feasibility and usefulness of IRAC data to these limits over the HUDF and GOODS-S. Even though less than 10\%  ($<70$ hour) of the program was executed before the program was terminated due to scheduling conflicts, the program was successful in one aspect. By placing the observations on areas with the deepest overlapping coverage from archival data, it produced the first $>150$ hour deep data in two separate 25 arcmin$^2$ fields in the central part of GOODS-S.\\

\subsection{Archival data}

Apart from the IGOODS and IUDF programs, there exists a wealth of ultradeep IRAC archival data from various programs (most of which are discussed in, e.g., Ashby et al. 2013, Ashby et al. 2015\footnote{We
note that Ashby et al. (2015) present different reductions of very similar observations as described here. We note several key differences: 1) we do not include the shallow and wide field PID 81 and PID 20708 data, but we do include the deep IGOODS PID 10076 observations, 2) reduction and interpolation method are a weighted sum on 0\farcs6 pixel scale in Ashby et al. (2015) versus Drizzling on 0\farcs3 here, and 3) the release in this paper of PSF maps corresponding to the reduced mosaics.}). Table \ref{tab:observations} provides an overview of the programs, the respective PIs, the number of exposures and total integration time. We downloaded all data from the Spitzer Heritage Archive and combined them with our data sets, reducing all in a consistent manner, and coadding them into one ultradeep mosaic. The 7 programs are divided up in 353 Astronomical Observation Requests (AORs), consisting of 33439 exposures, and totaling 3.47 Ms (962.6 hours) in each of the $3.6\mu m$\ and $4.5\mu m$\ filters for a total of 1925 hours of IRAC data. At the deepest location the coverage reaches $\sim220$ hours at $3.6\mu m$\ and $\sim190$ hours at $4.5\mu m$\ over an area of $\sim5$ arcmin$^2$. \\

\section{Reduction}

The reduction of the IRAC data was carried out starting with
the corrected Basic Calibrated Data (cBCD) generated by the Spitzer
Science Center (SSC) calibration pipeline. A custom
pipeline written by IL was used to post-processes and mosaic the
cBCD frames. The reduction pipeline was also used for reducing
the SIMPLE IRAC Legacy Survey (PI van Dokkum) and described in
detail in Damen et al. 2011.\\

\subsection{IRAC Reduction Process}
The reduction uses a two pass procedure. The first pass comprises
background structure removal, artifact correction, persistence masking,
and a first-pass coaddition. First, a median image is constructed from all
frames in the AOR, to remove background or bias structure and artifacts,
and it is subtracted from each frame\footnote{This procedure works well for
the IUDF, IGOODS, GOODS, and UDF, which take one frame per dither position, but not
for SEDS, S-CANDELS, and ERS, which make use of in-place repeats. This leads to
different bias patterns in the ``first frame'' and the ``repeat frame'' of
each dither. We subtract these by creating two median images, one for all first frames
and one for all repeat frames. }. Then the cBCDs are inspected and
additional artifacts are corrected.  The most important effect is residual
column-pulldown and pull-up. The pull-up/down, caused by bright stars or cosmic
rays at levels $> 10-20$ MJy/Sr in $3.6\mu m$\ and $4.5\mu m$, shifts the intensities
of the column above and below in slightly different ways. We correct for it
by subtracting a median above and below the affected pixels after excluding
any sources. Persistence from very bright stars, leaving
positive residuals on subsequent readouts of the array, is masked by rejecting
all highly exposed pixels in the subsequent 4 frames ($\approx400s$).
A constant background pedestal is determined and subtracted from each frame,
 by iteratively masking pixels associated with sources
 and determining the mode of the remaining background pixels.

Finally the post-processed cBCD frames of each AOR are registered and median combined
and a Median Absolute Deviation (MAD) map is calculated (reflecting the uncertainty in
the combined output pixels). The data are very well dithered, hence the images are free
from deviant pixels and can be used to create an object mask.

The second pass comprises cosmic ray rejection, astrometric calibration,
background structure removal, and a final coaddition. First, the first-pass median image is
de-registered and subtracted from each frame. The difference images are divided by
the MAD uncertainty image and used as detection maps for cosmic rays and hot/cold pixels.
Pixels are flagged if they deviate more then 4.5$\sigma_{MAD}$, while pixels adjacent
to outliers are iteratively clipped at a more aggressive $>2.5\sigma_{MAD}$ threshold.
The first-pass image is also used to calibrate the astrometry. The frames in an AORs
are corrected for a simple shift in RA and Dec using sources in common
with the deep WFC3 maps of 3D$-$HST (Skelton et al. 2014). These maps are
convenient as they include the WFC3 observations of the CANDELS/GOODS-South, the WFC3 ERS,
and the HUDF + parallel fields. The rms residuals of individual IRAC
source positions is $0\farcs05-0\farcs07$ rms with systematic
differences on scales of a few arcmin of $\lesssim0\farcs02$. The Skelton et al. (2014)
astrometry was calibrated to the CANDELS/GOODS-South (Koekemoer et al. 2011) mosaics
and to the GEMS (Rix et al. 2004) mosaic for the HUDF parallel fields.

\figpsf
\figpsfmap

A new median background structure map is created from all frames in the AOR,
this time masking objects and outlier pixels. The frames  are then drizzled
(Fruchter \& Hook 2002) per AOR using a pixfrac=0.2 on reference grid defined
by the CANDELS tangent point and a fine $0\farcs3$ pixel scale. A final background
was subtracted by iteratively clipping pixels belonging to objects and subtracting
the mode of the background pixels. Finally, the AORS are weighted
by the exposure time per pixel and combined into the ultradeep mosaic.
The cryogenic observations (GOODS and UDF2) data sets at $3.6\mu m$\ are $\sim$30\%
more sensitive than those of the warm mission hence we increase their contribution
to the final mosaic and exposure time maps by a factor 1.7.
There are no significant differences in sensitivity in $4.5\mu m$.
The data release includes the full-depth mosaics in both $3.6\mu m$\ and $4.5\mu m$,
as well as mosaics for each AOR in both filters (353 total, on the same grid
and final mosaic position angle). \\

\figmosaic
\figcoverage

\subsection{Point-Spread Function (PSF) Construction}
Accurate point spread functions are needed to facilitate IRAC photometry
using PSF fitting techniques or using the high resolution HST imaging
as a prior. Empirical PSFs created from the reduced mosaics are
preferable, as the observation and reduction processes change the PSFs in subtle ways.
However, extracting clean PSFs to large radii and high dynamic range
is challenging due to crowding of neighboring sources
and the small number of stars usually available in deep blank fields.
To complicate matters, the layout and different rotation angles of the AORs
cause the effective PSF of the combined mosaic to change
rapidly on small spatial scales.

\figcol
\figexptime
\figimprovement

To solve this we generate a spatially varying IRAC PSF. First we take
advantage of the optical stability and the fine sampling to generate
one template ``super PSF'' at $3.6\mu m$\ and $4.5\mu m$. Two hundred stars were
identified in deep HST imaging based on their FWHM and magnitude
(e.g., Skelton et al. 2014) and requiring an axis ratio of $b/a>0.85$.
At corresponding locations in each of the 353 AOR mosaics (which are
on the same grid and PA as the full-depth mosaic), image stamps of the
stars were extracted to $R=20\arcsec$ radius. Saturated star images
and those with $SNR<300$ were rejected. The remaining 2050 star images
were then rotated to the native orientation of the IRAC frames to
align the PSF features. Subsequently the images were normalized and
median stacked, sigma clipping outlier pixels due to neighboring
objects. The stacking was iterated three times while growing the
outlier masks by 1 pixel in each iteration. Note that some stars are
imaged in more than 100 distinct AORs. Therefore the distribution of
position angles causes objects close to the stars to fall on different locations on the
IRAC frames. This makes it easier to separate between true PSF
structure and faint signal from neigboring sources, turning the
complex nature of the observations into an asset.

The resulting template PSFs are shown in
Figure \ref{fig:psf} and are of much higher quality and SNR than usual for
deep extragalactic fields. The drizzling on a fine pixel scale of
$0\farcs3$ helps to recover high frequency features of the PSF,
while the large number of high SNR images results in a dynamic range of
$>10,000$.

The second step is to combine the template PSF in such a way that
simulates the combination of the AOR into
the full-depth mosaic. We map the exposure time and rotation
angles of each AOR on a fine grid ($12\arcsec$) covering the output image.
Then we reconstruct the effective full-depth PSF, by rotating\footnote{Rotation and bicubic interpolation of the template PSF introduces very slight smoothing, but is
does not affect the photometry ($<0.2\%$ at small radii).} and weighting the template PSF for each AOR contributing to that grid location.

Figure \ref{fig:psfmap} shows the reconstructed PSFs in
steps of $2.5$ arcmin, illustrating the strong spatial variation. Bootstrap
resampling the star list and repeating the process results in uncertainties
much smaller than the spatial variation in constructed PSF. This indicates
that survey geometry has a much larger impact on the effective IRAC PSF
than the intrinsic variation of the PSF over a single IRAC pointing.
Both the super PSFs and the maps are made available in the data release.

\section{Results}
\subsection{Reduced Image Properties}
The reduced IRAC mosaics are shown in Figure \ref{fig:mosaic} and the
corresponding coverage maps are shown Figure \ref{fig:coverage}. A color
composite using $K_s-$band, $3.6\mu m$\, and $4.5\mu m$\ is shown in Figure \ref{fig:col}.
The combined observations of all previous programs results in extremely
deep coverage, due in part to targeted observations over the HUDF/XDF
from the IUDF and IGOODS programs, and in part from fortuitous
overlap from archival data. The uncoordinated nature of the programs
is revealed by the much smaller area covered in both filters
simultaneously: the area is smaller by a factor of $>2$ at $>100$ hr
and factors of $>5$ at $>150$ hours). Simultaneous coverage is
crucial for placing constraints on emission line strengths and
stellar masses at $z>7$ (e.g., Labb\'e et al. 2013). Presently, two small
ultradeep ($180-200$ hr) areas in GOODS-S exist (9 arcmin$^2$ in
$3.6\mu m$\ and $4.5\mu m$\ each).

\figdiag

The final mosaics are cosmetically clean and the background
is flat to $5\times10^{-5}$MJy sr$^{-1}$ ($\sim$31 mag/arcsec$^2$ AB)
on scales of $1$ arcmin. The small area that reaches to $180-200$ hours
allows us to evaluate the improvement in background noise relative to the existing deep $25$
hour integrations. As illustrated in Figure \ref{fig:improvement}
the improvement is obvious in both IRAC bands, with large increases in
the number of detected ultrafaint sources and in the SNRs of brighter objects.

The image quality of the full depth mosaics is excellent and constant over the field. The 1-D gaussian full-width at half-maximum (FWHM) over the field
is $1\farcs49\pm0.015$ at $3.6\mu m$\ and $1\farcs48\pm0.025$ at $4.5\mu m$. These
values are identical to those of the cryogenic GOODS v0.3 public data release,
and 20\% smaller than those of the SEDS (PID 60022; Ashby et al. 2013) and
SIMPLE mosaics (PID 20708; Damen et al. 2011). The difference with the latter
two programs is due to the native IRAC pixels undersampling the PSF and using
drizzling instead of interpolation when resampling the IRAC frames.

We verify the photometric calibration by comparing the fluxes of bright sources
($<20$ mag AB) in $5\arcsec$ diameter aperture to earlier measurements. The
agreement with the IRAC $3.6\mu m$\ and $4.5\mu m$\ imaging of the Spitzer Extended
Deep Survey (SEDS; Ashby et al. 2013) is excellent ($<1\%$ offset).
Comparing to cryogenic GOODS-S imaging (PID 194, PI Dickinson, data release DR3)
reveals that the GOODS fluxes are brighter by 8\% and 2\% in $3.6\mu m$\ and $4.5\mu m$\
respectively. This is due to a change in BCD pipeline calibration: the
FLUXCONV values reported in the PID 194 headers (GOODS DR3, v0.30/v0.31,
BCD pipeline S10.5.0) are 7\% and 1\% brighter than the FLUXCONV values in the
most recent calibrations of the same data (BCD pipeline version S18.25.0).
Comparisons to our own reduction of the recalibrated GOODS data shows no offset.

\subsection{Photometry and Confusion}

The total integration times of the mosaics ($50-200$ hours) run well into the classical ``source confusion'' regime for low background extragalactic observations, where crowding by nearby sources affects the reliability of photometry. The classical confusion limit predicted by Franceschini et al. (1991) is $0.6\mu$Jy ($24.5$ AB mag), but in reality confusion is not a hard limit. For example, the classical limit is strictly speaking not relevant when the positions of the sources are known a priori. In GOODS-South and the HUDFs deep ($H_{AB}=27-30$), high-resolution (FWHM$=0\farcs16$) HST/WFC3 imaging is available and the IRAC images are registered to the WFC3 images to very high accuracy ($\lesssim0\farcs02$ systematic). Using the source positions and sizes in the high resolution image, combined with knowledge of the PSFs of WFC3 and IRAC, it is possible extract the source flux by modeling the IRAC surface brightness distribution.
Although surface brightness distribution can vary with wavelength, such procedures already greatly reduce the effect of confusion and open up the possibility of extracting fluxes well beyond the classical limit.

Prior based photometric techniques on blended sources and multi-resolution data sets have been used by many groups in the past with good results (e.g., Fernandez-Soto et al. 1999, Papovich et al. 2001, Shapley et al. 2005, Labb\'e et al. 2005,2006,2010,2013, Grazian et al. 2006, Wuyts et al. 2007, DeSantis et al. 2007, Laidler et al. 2007). As demonstrated in Figure \ref{fig:diag} these techniques can work extremely well.  Note that the photon noise for most sources is negligible compared to the background noise. Therefore, when sources can be modeled and subtracted perfectly, most of the field can be considered empty sky from the perspective of faint source detection.

While good results can already be obtained by simple PSF fitting (i.e., assuming point sources and a negligible size of the high resolution WFC3 PSF), for the best results and smallest residuals near the cores of bright sources, it is necessary to account for both the source size and the detailed shape of the WFC3 and IRAC PSF. This can be done by convolving the isolated high resolution object by a kernel, constructed by deconvolving the low resolution PSF by the high resolution PSF (e.g., Labb\'e et al. 2003, Labb\'e et al. 2005). \\

\fignoise
\figdepth

\subsection{Depth}

The large variation in integration time makes it possible to study the relation between sensitivity and integration time using prior based photometry.  We measure the sensitivity limits of the IRAC images by placing artificial sources of zero flux on 15,0000 random locations in the mosaic and extracting their flux using the WFC3 image as a prior, as previously described and shown in Fig. \ref{fig:diag}. To enable straightforward comparisons with other noise measurements, we do not use the best-fit flux directly but subtract the best-fit model of all neighbors to give a ``cleaned'' image of the source. Then we measure the unweighted flux in $D=2\farcs0$ diameter circular apertures (without further corrections for light outside the aperture).

The histograms of extracted fluxes are shown in Figure \ref{fig:noise}), grouped in bins of integration time. As expected, the scatter histogram becomes progressively narrower with increasing integration time, with no evidence for bias even at the largest integration times.
To compare to the scatter expected from pure background noise, we compute for each fake source the local background RMS in empty regions of the residual image (away from bright sources). We bin by $6\times6$ pixels ($1\farcs8\times1\farcs8$) to approximate the area of a $D=2\farcs0$ aperture. The local empty background RMS is optimistic and only representative of the uncertainty in absence of confusion. As shown in Figure \ref{fig:noise}) ({\em right}) the two estimates agree very well for 90\% of the sources: the histogram of the ratio of aperture flux to local background error resembles a standard normal \hbox{$\mathcal{N}$}$(0,1)$\ distribution. There is a slight skew towards positive flux levels, indicated by excess positive residuals for $\sim5\%$ of the sources in the $2-3\sigma$ range. About $12\%$ of the fluxes deviate by more than $5\sigma$ (10\% high, 2\% low), nearly all due to strong residuals near the centers of very bright IRAC sources. About $3\%$ deviate because of confusion in the high resolution WFC3 prior image.

We further investigate the relationship between contamination fraction and integration time,
defining ``strongly contaminated'' as $>5\sigma$ deviations from the local empty background RMS. Using simple aperture photometry (e.g., SExtractor) on the full-depth mosaics we find high contamination fractions: $\sim80\%$ at $3.6\mu m$\ and $\sim70\%$ in $4.5\mu m$. There is only a weak trend of contamination with integration time, likely because most flux comes from moderately bright sources and the PSF surface brightness profile is steep at small radii $R<10\arcsec$ (e.g., Spitzer Observer Manual, SOM, section 6.2.4.1.5). For the cleaned photometry there is no trend with integration time over $20-200$ hour (and a constant $\sim12\%$ contamination). Hence prior based cleaning reduces the contamination fraction for these data sets by a constant factor $6\times$.

Figure \ref{fig:depth} shows the relation between sensitivity and integration time based on the simulated sources. The noise decreases with a power-law slope of $t_{exp}^{-0.45\pm0.01}$ in both IRAC bands. The decrease is only slightly slower (at $2.5\sigma$ significance in each filter) than the $\sqrt{t_{exp}}$ expected for poisson noise. Following the definition of the IRAC integration time calculator (SENS-PET), we convert aperture scatter to point source sensitivity by square root scaling the noise to an equivalent area of $10.5~$arcsec$^2$. This area represents the number of  ``noise pixels'' (see SOM Table 6.1), which would effectively contribute to the uncertainty of linear least-squares fit of a point source. This amounts to optimal weighting by the PSF and improves the SNR by $\sim30\%$ compared to unweighted apertures.\\

The best fit in magnitudes is:
\begin{equation}
 \text{mag}(3.6\mu m,1\sigma,AB) = 25.81 + 1.132 \log_{10}{t_{exp}}
\end{equation}
\begin{equation}
 \text{mag}(4.5\mu m,1\sigma,AB) = 25.66 + 1.141 \log_{10}{t_{exp}}
\end{equation}

or equivalently in flux densities:

\begin{equation}
 \sigma(3.6\mu m,nJy) =   172 * t_{exp}^{-0.453}
\end{equation}
\begin{equation}
 \sigma(4.5\mu m,nJy) =   197 * t_{exp}^{-0.456}
\end{equation}

which gives the median point source sensitivity as function of integration time in hours.
No evidence is found for a confusion limit or noise floor, although the relation is consistently $10-30\%$ less deep than predicted by SENS-PET for low background conditions. A possible explanation for the lower sensitivity is residual confusion by, e.g., sources below our detection limit or a background of faint overlapping PSF wings at larger radii than our PSF model. Note that the true uncertainty for individual sources can be much higher than the median if the source is located close to a bright neighbor. \\

\subsection{Public Data Release}
The data release consists of reduced images of all ultradeep IRAC observations in the GOODS-South. The images are available from the IUDF website\footnote{\url{http://www.strw.leidenuniv.nl/iudf/}} and the Infrared Science Archive\footnote{ \url[http://irsa.ipac.caltech.edu/data/SPITZER/IUDF/]{http://irsa.ipac.caltech.edu/data/SPITZER/IUDF} } (IRSA).\\

The data release contains the following:
\begin{itemize}
\item Science images and exposure time maps in both $3.6\mu m$\ and $4.5\mu m$. Our reduction uses the same tangent point as CANDELS on pixel scales of $0\farcs3$, so the IRAC maps can be easily rebinned and registered to HST/WFC3 data.

\item Reduced images of all individual 353 AORs, drizzled onto the same grid, which may be useful to study the reliability or variability of sources.

\item Template PSFs and spatial maps of the weights and position angles of each AOR, allowing the reconstruction of the PSF at arbitrary locations. Example IDL code is provided.
\end{itemize}

The units of the science images are $c $MJy/sr, where constant
c=16.54 represents the change from the native IRAC pixel
scale to 0.3"/pixel due to flux conservation during the reduction process.
Equivalently, flux densities can be obtained by multiplying the image pixel values by
34.994 $\mu$Jy/pixel, corresponding to an image AB zeropoint of 20.04.\\

\section{Examples}

One of the main goals of the IUDF program is to obtain high SNR ($>5\sigma$)
at $3.6$ and $4.5\mu$m for normal $\lesssim L^*$ galaxies in the epoch of reionization.
Comparing the detection rates of $H<27.5$ galaxies at $z>6$ to previous deep IRAC
observations from the GOODS program (PID 194), we find that $\sim46$ hour
GOODS data yields SNR$>5\sigma$ measurements for 25-30\% of the sources,
compared to 75-80\% for $150-200$ hour in the IUDF images.

Here we provide several examples of objects detected in the IUDF images. In Figure \ref{fig:highz}  we show 4 ultrafaint sub-L* galaxies at $z\sim7-8$.  The galaxies are clearly detected at high significance in the new images, compared to the earlier 50 hour deep images. In the deeper images a clear difference in observed IRAC color is seen between the $z\sim7$ and $z\sim8$ galaxies, likely due to  strong [\ion{O}{3}]+$H\beta$ line emission moving from $3.6\mu m$\ to $4.5\mu m$\ with increasing redshift. These differences were recently demonstrated in stacked SEDs (e.g., Labb\'e et al. 2013) and in small samples of brighter and lensed galaxies (Smit et al. 2014, Smit et al. 2015), but are now apparent even in individual sub-L* galaxies. This shows the potential of $\sim150-200$ hour data
for placing improved constraints on the emission line strengths of individual galaxies ($H\alpha+$[\ion{N}{2}] at $z=4-5$ and [\ion{O}{3}]+$H\beta$ at $z=7-8$).

\fighighz

Furthermore, ultradeep IRAC data may be the only way to detect potentially important overlooked constituents of the high redshift universe until the arrival of JWST. Massive M$\gtrsim 10^{10}$M$_\odot$ passive galaxies at $z>4$ can be too faint to be detected by Hubble and even actively star forming, dusty galaxies with SFR $50-100$M$_\odot$/yr could have escaped detection by both Hubble and existing FIR/sub-mm surveys at these redshifts. Enigmatic IRAC-selected ``HST-dropouts'' have been identified on the basis of their very red $H-4.5$ colors (e.g., Huang et al. 2011, Caputi et al. 2013). The origin of these objects is unknown as it is difficult to determine their redshifts, but the observed SEDs of some galaxies can be fit with quiescent galaxy models at high redshift $z>4$. If this interpretation is correct, then these objects are the quenched remnants of massive starbursts at earlier times, and they provide compelling targets for early JWST spectroscopic follow up. Such a population likely places powerful constraints on models for star formation quenching, and may inform us indirectly about high mass star formation during the epoch of reionization. \\

\section{Summary}

The IUDF and IGOODS programs are the deepest and most recent probes of the infrared emission at $3.6\mu m$\ and $4.5\mu m$\ with Spitzer/IRAC, ideally suited for faint studies of high redshift galaxies. Combining with all ultradeep archival data from all previous programs, and using consistent reduction procedures, we present reduced image mosaics reaching extremely deep coverage of $50-200$ hours and covering all of GOODS-S, the HUDF/XDF, and the two HUDF parallel fields. \\

In summary:
\begin{itemize}
\item We release the full-depth reduced science mosaics at $3.6\mu m$\ and $4.5\mu m$\, and the corresponding exposure time maps. The IRAC mosaics are placed on the same astrometric system and reference grid as the CANDELS WFC3 mosaics.\\

\item The combined mosaics are the deepest ever taken at $3.6\mu m$\ and $4.5\mu m$\, with the integration times ranging from $>50$ hour over $150$ arcmin$^2$, $>100$ hour over $60$ sq arcmin$^2$, to $\sim180-200$ hour over $5-10$ arcmin$^2$. The image quality is FWHM=$1\farcs49$ in both bands with $<1.5\%$ spatial variation.\\

\item The release also includes the separate reduced mosaics of all individual 353 AORs of the 7 programs involved in this release, registered and drizzled onto the same grid, to study the reliability or variability of sources.\\

\item We present a new procedure to construct IRAC PSF maps from the data, well suited to deep fields with relatively few bright stars and complicated survey geometry with repeat observations onder varying roll angles. The PSF maps are included in the release to facilitate PSF-fitting or joint IRAC+WFC3 photometry.\\

\item Simulations are performed to quantify the confusion due to crowding by neighboring sources.
We demonstrated using the new ultradeep 200 hour data that IRAC observations are not significantly impacted by confusion when using deep high resolution priors from HST/WFC3. In the reduced mosaics $70-80\%$ of the area is originally contaminated by flux of neighboring sources. Using HST-based priors reduces this to a constant $\sim12\%$, with no dependence on exposure time over the range $20-200$ hours. The remaining catastrophic outliers are nearly all very close to the centers of bright IRAC sources and in $3-4\%$ are even confused in the high resolution HST image. In general, prior based photometry works very well, reducing the contamination fraction by $6\times$. \\

\item The simulations further demonstrate that the rms noise in the ultradeep IRAC images decreases nearly as the square root of integration time over the range $20-200$ hours, without any evidence for a hard confusion limit. The maximum  $1\sigma$ point source sensitivities reaches as faint as of 15 nJy (28.5 AB) at $3.6\mu m$\ and 19 nJy  (28.2 AB) at $4.5\mu m$. These sensitivities are systematically $10\% - 30\%$ less deep than predicted by the IRAC ETC (SENS-PET), likely due to residual effects of confusion. We provide fitting formulas in \S4.3 to estimate the effective depth as a function of exposure time.\\

\end{itemize}

The value of ultradeep IRAC data is illustrated by direct detections of sub-L* $z>7$ galaxies, where the joint measurement at $3.6\mu m$\ and $4.5\mu m$\ places  constraints on the [\ion{O}{3}]+$H\beta$   emission line strengths of individual galaxies to very faint limits $H_{AB}\sim28$. Future observations of larger samples over wider areas will become available as part of Exploration Science program GREATS (GOODS Re−ionization Era wide−Area Treasury from Spitzer, PI Labb\'e), which will map part of GOODS-S and GOODS-N to 200 hours depth. These data offer the prospect of studying the distribution of inferred EWs and comparions to the entire rest-frame SEDs, from HST to ALMA,  will enable studies of the dust attenuation, ionization processes, and star formation histories. The combined HST+Spitzer ultradeep imaging legacy will be useful for planning efficient imaging and spectroscopic follow-up surveys with JWST and provide interesting targets for the first cycles of JWST NIRSPEC observations. Spitzer's heritage will extend well into the JWST era.

\acknowledgements

We thank the anonymous referee for careful comments which improved the clarity of
the paper. We thank Justin Howell for IPAC assistance with the data release.
Support for this work was provided ERC grant HIGHZ no. 227749 and NL-NWO Spinoza.
We acknowledge support from NASA grants NAG5-7697 and HST-GO-11563.
This research has made use of the NASA/ IPAC Infrared
Science Archive, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration.


I am writing this letter for requesting you to allow leave for a week to my son John Perry studying in nursery in your class.
Jon's father has been hospitalized yesterday. He is advised to be operated day after tomorrow as he met with a severe accident yesterday. All this process will at least take a week. During this time, it would not be possible for John to attend school as the whole family will be occupied in the hospital and no one will be able to look after her or get her ready for school.
Therefore I request you to grant leave for a period of a week from today 4th February 2012.


Make it Personal – and Interactive!
A website that is interactive and proactive – it doesn't just sit there waiting for its users to take action – is a key component of the success of many online businesses. It doesn't matter if you are selling business-to-business or consumer goods or services, online shoppers tend to have short attention spans and you have to do everything you possibly can to capture and keep your website's visitors interest. Just like a charming and friendly salesperson, an interactive website helps your users to develop a more personal connection with your website and your business.
Live chat software from ChatWare can be an excellent way to bring better interactivity and user engagement to any website. Chatware gives your users the ability to immediately interact with a representative of your company, and offers people the opportunity to immediately ask questions, voice concerns, and know that real people at the company are accessible any time of day. It's may seem like cold digital world, but customers really warm up to the idea of having a real person to deal with. Pre-sale or post-sale, the feeling of connection that live chat gives your customers – along with your own personal touch in customer service – just may be that one thing that keeps them coming back.
Using live chat to enhance your website is just the beginning. Upwards of 60% of all web usage now happens on mobile devices – iPhones, Androids, tablets, and so on. The web isn't just on the desktop PC anymore – it is right in your customers' hands wherever they are. Chatware's innovative and very useful Text to Chat feature allows your customers to initiate a chat on whatever device they choose whether it is a smartphone or that good old desktop PC.
If you would like to learn more about how Chatware's dedication to constantly improving our chat products can help enhance and improve your online presence, call 1-800-601-0693, or contact Chatware right now to get started.


Health and fitness Instruments help you produce clever wellbeing choices or simply get it done to enhance your health.
Decision Points concentrate on crucial expenses conclusions that will be important to a number of health problems.
Semilunar cartilage Split: Breath analyzer Have a very good Diagnostic assay (MRI or Arthroscopy)?
Meniscus Bust: Breath analyzer Include Surgery?
Actionsets are designed to aid persons get a vigorous function during managing a health condition.
This information does not take the place of counsel associated with a doctor. Healthwise disclaims virtually any warranty or simply burden to use of this facts. Ones own make use of this information will mean that anyone admit the actual Relation to Apply. The correct way these details was made that will help you make smarter health and wellbeing decisions.
© 1996-2014 Healthwise, Integrated. Healthwise, Healthwise per wellness verdict, along with the Healthwise business logo tend to be art logos associated with Healthwise, Designed.
Vermox (mebendazole) Drug Adverse reactions, Friendships, and Prescription medication Information on World-wide-Medicalsearch.


text:
Croke Passes Measure Combatting Organized Retail Theft, Fights for Public Safety
Apr 14, 2022 | Croke
CHICAGO, Ill. – Following her ongoing efforts to keep her community safe from the threat of violent crime, state Rep. Margaret Croke, D-Chicago, passed legislation cracking down on organized retail theft. It is now headed to the Governor's desk for signature. "As our...
Croke Works for Public Safety, Combats Dangerous Growth of Street Racing, Car Stunts
Mar 23, 2022 | Croke
CHICAGO, Ill. – Continuing her efforts to improve public safety, state Rep. Margaret Croke, D-Chicago, recently helped pass a measure to cut down on street racing and dangerous stunts also known as 'street sideshows', which put lives at risk. "By disregarding speed...
Croke Combats Theft of Catalytic Converters, Works for Public Safety
CHICAGO, Ill. – In a continued effort to promote public safety, state Rep. Margaret Croke, D-Chicago, backed a measure to combat the theft of catalytic converters currently plaguing Illinois drivers. "Public safety is a priority for me, and improving that requires a...
Croke Responds to Governor's Address, Remains Focused on Honoring Fiscal Commitments, Keeping Illinois Families Safe
Feb 3, 2022 | Croke
CHICAGO, Ill. – State Rep. Margaret Croke, D-Chicago, issued the following statement Wednesday after Gov. J.B. Pritzker's annual budget address: "As we go to the negotiating table to craft the next budget, I want my priorities to be clear: we must fully fund pensions,...
Croke Works for Ethics Reform, Government Transparency
Jun 8, 2021 | Croke
SPRINGFIELD, Ill. – New ethics standards and government transparency requirements that have long been needed in Illinois will be made law under legislation State Rep. Margaret Croke, D-Chicago, helped pass. "Public trust in elected officials is critical and I'm...
Croke Fights for Affordable Health Care and Technology Advancements during Spring Legislative Session
SPRINGFIELD, Ill. – State Rep. Margaret Croke, D-Chicago, issued this statement following the completion of the 2021 spring session: "Despite the challenges of this session, I'm proud to say I, along with my colleagues, have made great strides towards overcoming the...

redpajama_set_name: RedPajamaCommonCrawl


text:
Introduction of 24 h resident consultant cover in a tertiary neonatal unit—impact on mortality and clinical outcomes
Carolina Zorro, Theodore Dassios, Ann Hickey, Anusha Arasu, Ravindra Bhat, Anne Greenough
https://doi.org/10.3390/children8100865
Funding Information: Funding: The research was supported by the National Institute for Health Research (NIHR) Biomedical Research Centre based at Guy's and St Thomas' NHS Foundation Trust and King's College London. The views expressed are those of the author(s) and not necessarily those of the NHS, the NIHR or the Department of Health. Funding Information: The research was supported by the National Institute for Health Research (NIHR) Biomedical Research Centre based at Guy?s and St Thomas? NHS Foundation Trust and King?s College London. The views expressed are those of the author(s) and not necessarily those of the NHS, the NIHR or the Department of Health. Publisher Copyright: © 2021 by the authors. Licensee MDPI, Basel, Switzerland.
King's Authors
Ravindra Bhat (Child Health Clinical Academic Group)
Anne Greenough (Women & Children's Health, Child Health Clinical Academic Group, Allergy Respiratory Critical Care Anaesthetics and Pain Therapies Clinical Academic Group)
Background: We aimed to determine whether the introduction of 24 h cover by resident consultants in a tertiary neonatal unit affected mortality and other clinical outcomes. Methods: Retrospective cohort study in a tertiary medical and surgical neonatal unit between 2010–2020 of all liveborn infants admitted to the neonatal unit. Out of hours cover was rearranged in 2014 to ensure 24 h presence of a senior trained neonatologist (resident consultant). Results: In the study period, 4778 infants were included: 2613 in the pre-resident period and 2165 in the resident period. The median (IQR) time to first consultation by a senior member of staff was significantly longer in the pre-resident period [1.5 (0.6–4.3) h] compared to the resident period [0.5 (0.3–1.5) h, p < 0.001]. Overall, mortality was similar in the pre-resident and the resident periods (3.2% versus 2.3%, p = 0.077), but the mortality of infants born at night was significantly higher in the pre-resident (4.5%) compared to the resident period (2.5%, p = 0.016). The resident period was independently associated with an increased survival to discharge (adjusted p < 0.001, odds ratio: 2.0) after adjusting for gestational age, admission temperature and duration of ventilation. Conclusions: Following introduction of a resident consultant model the mortality and time to consultation after admission decreased.
Chronology and Determinants of Respiratory Function Changes Following Administration of Systemic Postnatal Corticosteroids in Extremely Preterm Infants
Dassios, T., Kaltsogianni, O., Hickey, A., Bhat, R. & Greenough, A., 1 Dec 2019, In: Journal of pediatrics. 215, p. 17-23 7 p.
Prediction of Mortality in Newborn Infants With Severe Congenital Diaphragmatic Hernia Using the Chest Radiographic Thoracic Area
Dassios, T., Ali, K., Makin, E., Bhat, R., Krokidis, M. & Greenough, A., 1 Jun 2019, In: Pediatric critical care medicine : a journal of the Society of Critical Care Medicine and the World Federation of Pediatric Intensive and Critical Care Societies. 20, 6, p. 534-539 6 p.
Neonatal chylothoraces: a 10 year experience in a tertiary neonatal referral centre
White, M. K., Bhat, R. & Greenough, A., 13 Mar 2019, In: Case Reports in Paediatrics.
The effects of sleeping position, maternal smoking and substance misuse on the ventilatory response to hypoxia in the newborn period
Rossor, T. E., Ali, K. A. M., Bhat, R., Trenear, R., Rafferty, G. & Greenough, A., 6 Jul 2018, In: Pediatric Research.
Detection of gastro-oesophageal reflux on the neonatal unit
Rossor, T., Lingam, I., Douiri, A., Bhat, R. & Greenough, A., 13 Mar 2018, (E-pub ahead of print) In: Acta Paediatrica.
With some of the same researchers
Carboxyhaemoglobin levels and free-radical-related diseases in prematurely born infants
Bednarczuk, N., Williams, E. E., Greenough, A. & Dassios, T., Jan 2022, In: Early Human Development. 164, 105523.
Nicotine replacement therapy and e-cigarettes in pregnancy and infant respiratory outcomes
Bednarczuk, N., Williams, E. E., Dassios, T. & Greenough, A., Jan 2022, In: Early Human Development. 164, 105509.
Survey of bi-level continuous positive airway pressure in UK neonatal units: UK survey of BiPAP use
Bednarczuk, N., Williams, E., Gunawardana, S., Arattu Thodika, F. M. S. & Greenough, A., Jan 2022, In: Acta Paediatrica. 111, 1, p. 99-100 2 p.
Respiratory Support of Infants With Congenital Diaphragmatic Hernia
Williams, E. & Greenough, A., 24 Dec 2021, In: Frontiers in Pediatrics. 9, 808317.
Pulmonary hypertension in infants with bronchopulmonary dysplasia: risk factors, mortality and duration of hospitalisation
Arattu Thodika, F. M. S., Nanjundappa, M., Dassios, T., Bell, A. & Greenough, A., 1 Dec 2021, (E-pub ahead of print) In: Journal of Perinatal Medicine.
Current practices on diagnosis, prevention and treatment of post-transplant lymphoproliferative disorder in pediatric patients after solid organ transplantation: Results of ern transplantchild healthcareworking group survey
Baker, A., Remacha, E. F., Canizales, J. T., Bravo-Gallego, L. Y., Fitzpatrick, E., Melgar, A. A., Bartolo, G. M., Guereta, L. G., Boluda, E. R., Mozo, Y., Broniszczak, D., Jarmużek, W., Kalicinski, P., Maecker-Kolhoff, B., Carlens, J., Baumann, U., Roy, C., Chardot, C., Benetti, E., Cananzi, M. & 18 others, Calore, E., Dello Strologo, L., Candusso, M., Lopes, M. F., Brito, M. J., Gonçalves, C., Do Carmo, C., Stephenne, X., Wennberg, L., Stone, R., Rascon, J., Lindemans, C., Turkiewicz, D., Giraldi, E., Nicastro, E., D'Antiga, L., Ackermann, O. & Vega, P. J., Aug 2021, In: Children. 8, 8, 661.
Prevalence and Associated Factors of Emotional and Behavioural Difficulties during COVID-19 Pandemic in Children with Neurodevelopmental Disorders
Nonweiler, J., Rattray, F., Baulcomb, J., Happe, F. & Absoud, M., 4 Sep 2020, In: Children (Basel, Switzerland). 7, 9


text:
using MvcView.Extensions;
using MvcView.Models;
using System.Data.Entity;
using System.Web.Mvc;
using System.Web.Optimization;
using System.Web.Routing;
using System.Web.WebPages;

namespace MvcView
{
    public class MvcApplication : System.Web.HttpApplication
    {
        protected void Application_Start()
        {
            //ViewEngines.Engines.Clear();
            //ViewEngines.Engines.Add(new WebFormViewEngine());
            //ViewEngines.Engines.Add(new RazorViewEngine());
            //ViewEngines.Engines.Add(new XslTransformViewEngine());
            AreaRegistration.RegisterAllAreas();
            FilterConfig.RegisterGlobalFilters(GlobalFilters.Filters);
            RouteConfig.RegisterRoutes(RouteTable.Routes);
            BundleConfig.RegisterBundles(BundleTable.Bundles);

            Database.SetInitializer<MvcViewContext>(new MvcViewInitializer());

            DisplayModeProvider.Instance.Modes.Insert(0,
              new DefaultDisplayMode("iPhone")
              {
                ContextCondition = (c =>
                    c.Request.UserAgent.IndexOf("iPhone") >= 0)
              });
        }
    }
}

redpajama_set_name: RedPajamaGithub


Info on sierra trading post coupons. Get Results from 8 Search Engines!
Save $$$ at Sierra Trading Post with coupons Enter your Sierra Trading Post key code or coupon code in the box and Sierra Trading Post Coupons & Promo Codes.
© Free location coupons Incorp coupon | Promo Codes & Deals 2018 Sierra trading coupon code.


text:
Checks Gold
Checks Gold app comes up with features to help you in keeping track of the received as well as issued checks. The scheduled section shows the date of the check, amount of the check, and sorts check according to the deadline date.
The app provides features through which you can also register all their current bank accounts so they can sort checks on the basis of accounts. The issued checks section shows the issue date of the check, cash date of the check, description of the check, and the amount of the check.
Checks Gold app also offers features that let you create a telephone directory so you can directly call your other users. You can tap on a contact to edit its details, to view it, or to delete it. You can turn on notification from the settings section to get alerts about check expiring.
Checks Gold Alternatives for Android
#1 Cheque-mate
Cheque-mate is an app by Ian Wong that comes up with features to help you in converting the numbers right on your mobile phone, so you can easily write Cheque. The options menu allows users to change settings such as the size of the font and the background color of the keyboard. The app provides features through which users can enter the number of converting them to English as well as to Chinese words.
You can also access the options menu by tapping and holding the C key on the keyboard. Cheque-mate app offers a built-in keyword that contains a clear button through which you can clear all the written numbers. You can also tap on the back button in order to erase a word without much of a stretch. Users can change the language by tapping on the desired language from the side panel.
#2 PrinterShare Mobile Print
PrinterShare Mobile Print app allows users to print images, emails, attachments, contacts, web pages, and various other digital media. You can tap on the select button to connect to all the nearby printers. It allows users to view nearby Wi-Fi, nearby Bluetooth, and Direct USB connection, etc.
PrinterShare – Printing documents and photos app provides users with pictures, contacts, calendar, webpages, messages, and call log, etc. and you can tap on the desired section print without much of a stretch. It shows a notification whenever the sending and printing are done.
PrinterShare Mobile Print app also comes up with an options menu where you can choose the font size of the text, page margins, the orientation of the page, size of the page, printing mode, and duplex mode. Users can also choose the number of copies of each page as well as can select the range of pages.
#3 PrintEasy
PrintEasy app offers features that let you print right from your mobile phone with the options to adjust and configure all the printer settings. The home screen contains buttons to enable users to access the Gallery, PDF, web, cards, contacts, and compose sections. PrintEasy: Print Anything From Anywhere Easily app comes up with features to help users in finding the PDF document by applying filters like name, size, and date.
You can also create and save documents to print them later. It also allows users to configure the page settings such as size, orientation, number of copies, range of the page, print quality, and duplex mode, etc. PrintEasy app also provides users with printing features in more than eight different languages through which they can print out the desired stuff in various languages. You can also print business cards by selecting templates from an extensive collection.
#4 Check Printer+
Check Printer+ app enables users to write and print a Cheque by using any nearby wireless printer. You can write information on the Cheque such as date, amount, name, bank address, zip code, memo, and signatures. Users can also search for the desired Cheque in the register by entering the Cheque number. The app offers features that let you automatically log all the written and printed Cheque so you can keep track of all your checks and account balance right at your fingertips.
The register shows the name of the payee, no of Cheque, date, memo, remaining account balance, and total debited amount. Check Printer+ app comes up with features to help users in printing blank Cheque by entering the starting check number, cutting line, and number of Cheque per page. You can change the font size, font, and bold, etc.
#5 Cheque Writer by OSO App
Cheque Writer is an app by OSO that provides features through which users can convert the text of Cheque into English and Chinese languages without much of a stretch. It also supports a large number so you can write as many numbers as you want to translate with a single tap.
The app allows users to enter the amount on the bar and tap on the convert button to view the given amount in Arabic numerals, English, and Chinese. You don't need an internet connection in order to convert the number into Arabic numerals, English numbers, and Chinese numbers.
Cheque Writer app also offers features that let you copy the text and written number directly from the convert section. It contains a straight forward interface that contains various sections to show the translation of the entered number in a large number of languages.
#6 Write a Check
Write a Check app comes up with an easy-to-use interface to help you in writing Cash Cheque in Dollars and cents. It also allows users to change the font settings by selecting the desired font as well as the desired size of the font right at your fingertips. The app provides a bar where you can write the desired number by adding full stops for cents. It shows the translation of the number before the full stop in the English language as well as the number after the full stop in numbers.
Write a Check app that offers features that let you tap on the back button to erase words without much of a stretch. You can also change the language by tapping on the desired language from the side panel. The home screen contains buttons to enable users to access the Gallery, PDF, web, cards, contacts, and compose sections.
#7 eSignPay
eSignPay app allows users to send credit card and check payment authorization requests so it can capture the payment after getting a signed payment authorization form. You can also change the electronic signature service by choosing the desired method from a list of more than six different electronic sign methods.
The home screen contains buttons to enable users to access eSign, Credit card sale, history, eCheck sale, account setup, and user guide sections. It provides you with settings section through which you can change the processing currency by choosing from more than eight currencies.
eSignPay app comes up with a built-in user guide that helps users in understanding and learning about how to use the app. The history section shows the names of payees, the amount credited, date of transactions, and type of payment methods. It also shows the total number of entries and the entries on the current page.
#8 US Routing Number Directory
US Routing Number Directory app offers features that let you quickly get details about the address of the desired branch of the bank so you can transfer funds without much of a stretch. It shows the area codes, and all the zip codes for the desired city, county, and state.
The app comes up with features to help users in getting the FEDACH routing details about banks such as zip code, telephone number, service number, and name of the city. The interface contains buttons to allow you to access details on the basis of Zipcode, bank details, FEDWIRE routing, and FEDACH routing.
US Routing Number Directory app also provides users with FEDWIRE routing details at a glance, including routing number of the bank, telegraphic name, FT status, FS status, and name of the state. You can also get details about all the branches of the desired bank in your city.
#9 Light Check
Light Check app enables users to create accurate images of checks from their checking as well as drafting bank accounts so they can pay by using remote deposit features. The app offers features that let you write a Cheque by entering the name of the recipient, total amount, memo, number of the Cheque, and Signature of the recipient.
Its interface contains buttons to allow users to view the back as well as the front side of the Cheque, and they can also get a new digital Cheque with a single tap. Light Check app comes up with features to help users in saving their account details, so they don't have to manually enter the information every time they want to pay someone. It shows a variety of different information on the Digital Cheque, such as date, address, memo, the amount in words, and amount in dollars.
#10 Eazycheque
Eazycheque is an app by Gulfpro Accountants that provide features through which users can print their Cheque in completely customizable formats right from their mobile phones. It also shows complete details about all the posted, upcoming, cleared, and overdue Cheque with actual numbers. The app allows users to view Cheque with date, name of the payee, total amount, and the currency of the Cheque.
You can tap on a Cheque in order to add it to cancel or clear the list with a single tap. It enables users to view upcoming all the upcoming Cheque. Eazycheque app offers a straight forward interface that lets you access postdated, upcoming, overdue, cleared, and canceled Cheque at a glance so you can keep track of your bank accounts. Users can tap on the view button in order to view the Cheque in the list as well as in block view.
#11 Number to Word Converter
Number to Word Converter app comes up with features to help you in converting large numbers into the western format. It enables you to write bank and financial Cheque by filling the bank slips with an accurate amount of deposited money in numbers as well as in words form.
The app provides features through which users can write large numbers, such as 100 digit numbers, to convert them into the words form. Its interface also contains buttons to allows you to add the currently converted number into a favorite list so you can also view it later.
Number to Word Converter app also offers features that let you copy and share the converted number with other users. You only need to enter the number on the bar and tap on the desired conversion method to get the up to 100 digit number into western as well as Indian format.
#12 ePic Check
ePic Check app allows users to use the mobile deposit functionality of all the major banks as well as financial institutions. It also shows you the tips for better images to keep track of all your financial transitions. Users can take pictures of back and front of the Cheque and can enter the account number to send payment.
The app comes up with features to help users in signing in to their ePic Check accounts so they can start depositing money to their bank account right away. The information section shows the address and contact information, such as telephone number, website, and directions.
ePic Check app also provides users with a competitive rate of banks so they can easily deposit large amounts of money by using the digital money depositing features. The home screen contains buttons to enable users to access information as well as all the previous digital payments records.
#13 Invoice Maker
Invoice Maker app offers features to lets you create, send, and track invoices so you can send estimates to your customers right through your mobile phone. Users can also use the search bar to search for the desired items, and it shows the frequently searched item on the top so they can easily add desired items to the invoice.
Invoice Maker: Estimate & Invoice App also provides features through which users can also get notification alerts when the client reads the invoice. The side panel allows users to access invoice, estimate, report, items, clients, accounts, and the settings sections.
Invoice Maker app also comes up with an invoice section where you can tap on the plus button to add new invoices in order to keep track of all your payments at a glance. Users can also add tax on items as well as on the total invoice.
#14 Typewriter
Typewriter is a virtual typewriter app that enables users to create masterpieces while enjoying the sound and the feeling of a real-life typewriter. You can also tap on the plus button in order to zoom in to the text or can tap on the minus button to zoom out.
The app comes up with features to help users in saving their work by tapping on the save button so they can easily access right from where they left. Its interface also contains buttons to allow you to translate the written text. You can also share the text directly from the writing screen with friends and family members.
Typewriter app offers features that let you change the color of the text and the color of the highlights, and they can also change the background color. Users can import an image from the phones' gallery to use it as a background image.
#15 Checkbook Plus
Checkbook Plus app provides features through which users can add and manage their daily transactions so they can track their every-day transactions right at their fingertips. It indicates credit funds in green color, debited funds in red, and level funds in white color.
The app allows users to schedule any recurring transactions, so they don't have to create transactions again and again. You can hide any secret transactions after transferring the funds. It also enables users to add a four-digit pin to keep their transactions secure. You can also export the set of data to backup and restore it.
Checkbook Plus app also offers features that let you tap on the plus button so you can add new transactions by entering the current and the available account balance. It also shows the date as well as the time of entry, the number of the check, and the modification date.
#16 Remplir Chèque
Remplir Chèque app allows users to easily fill their bank checks without getting help from any third parties. Its interface contains a button to enables you to share the amount of the Cheque with your friends and family members with a single tap.
The app comes up with features to enable users to write the amount of the Cheque in numbers, and it translates the amount into the English language. You can also tap on the volume button in order to get voice feedback after pressing each key on the keyboard.
Remplir Chèque app also provides users with a settings section where they can change the theme by choosing from a variety of different themes. You can also change the currency to write the checks in more than nine different currencies from around the world, including Euro, Dollar, Dinar, and Dirham, etc.
#17 Checkbook + Bank
Checkbook + Bank is a digital checkbook register app that offers features through which you can effortlessly manage your bank balance right on your mobile phone. The home screen contains buttons to allows users to receive checks, draw checks, deposit amount to the desired account and withdraw the amount from the desired account.
The app provides features through which users can easily track deposit and withdrawal of funds from their bank accounts as well as cash-boxes. The start section shows the total funds in banks and cash-boxes, as well as the amount received and sent through checks.
The search bar helps you in searching for the desired transactions with a single tap. Checkbook + Bank app comes up with features to help users in sorting checks by applying filters such as not cashed, cashed in banks, at the Bank, spent, date of the checks, and amount of the checks.
#18 Checks Gold Free
Checks Gold Free app enables users to monitor all their received and issued checks at a glance. Its interface contains an issued section where you can also view the cash date of the check, description of the check, and memo of the check, etc.
The app offers a schedule section where you can view the date of the check, total amounts of checks, as well as it also sorts all the checks on the basis of their deadlines so you can cash them first. You can tap on a contact to edit details such as name, email, and phone number.
Checks Gold Free app also comes up with features to help users in registering all of their bank accounts so they can manage and view checks according to the accounts. It also allows you to create and manage a digital telephone directory so you can dial calls to desired users.
#19 Cards Information Finder
Cards Information Finder app provides features through which you can find all the necessary information about credit and debit cards such as type of the card, name of the bank, name of the country, and name of the brand, etc.
The app enables you to enter only the first six digits of the number of the card to get all the information right on your mobile phone's screen. The top searched section shows the most searched bins by other users. You can also tap on the top searched bin to view all the information about them.
Cards Information Finder app offers an easy to use interface that contains a search bar where you can enter the bin number of the card and tap on the check button to view information. Users can also add bins to a favorite list to view them later.
#20 Simplest Checklist(check list)
Simplest Checklist(checklist) app is an app by JakiganicSystems that comes up with features to help you in creating simple checklists so you can organize your life. Users can also create new checklists by using voice input features.
The app offers a straight forward interface that contains a plus button that lets you add new checklists with a single tap. Users can tap on the delete button to delete any completed checklist. It also enables you to create customizable home screen widgets so you can view checklists at a glance.
Simplest Checklist (checklist) app provides features through which users can arrange and manage existing checklists by using drag and drop features. You can also delete existing checklists by using drag and drop features. Users only need to enter the name of the new checklist to create a new checklist without much of a stretch.
#21 IBAN Check IBAN Validation
IBAN Check IBAN Validation app allows users to check international bank account numbers so they can effortlessly send and receive payments. The help section shows all the rules with their details for the validation of the IBAN.
The app provides features through which you only need to enter the desired IBAN and tap on the check button to view the validation of the IBAN. It also enables users to share the results of the validation test of IBAN with other users as well as they can also copy it with a single tap.
IBAN Check IBAN Validation app also comes up with features to help users in entering the IBAN so they can also view the country of origin of the IBAN right on their mobile phones. The help section also shows all the supported countries with their ISO codes and the total number of characters of the IBAN.
#22 Credit Card Reader NFC (EMV)
Credit Card Reader NFC (EMV) is a digital banking card reader app that offers features through which you can hold your payment card to the back of your mobile phone, so you can get all the details about your card. The log section shows the log of the AID number, and you can share it with other users as well.
The app comes up with a straight forward interface that contains details, transactions, and log sections to show users all the details about the desired card at a glance. The detail section shows the type of the card, the total pin tries left, and AID number of the card.
Credit Card Reader NFC (EMV) app also provides users with a transaction section where they can view all the transactions according to dates, as well as it also shows the debited amount, type of the purchase, and the name terminal country.


EXQUISITE HIGHLY CARVED & PIERCED WIDE CHERRY AMBER Vintage BAKELITE Guaranteed Vintage Bakelite HINGED CLAMPER BANGLE BRACELET & MATCHING PIN, BROOCHTHIS WEEK! PLEASE NOTE: I strive to accurately describe all items to the best of my ability.
COLOR/ COMPOSITIONTRANSLUCENT CHERRY AMBER(GORGEOUS in SUNLIGHT) Vintage BAKELITEHIGHLY & DEEPLY PIERCED & CARVED rendered in an ORGANIC FLORAL or ACORNS MOTIF. MEASUREMENTSBRACELET MEASURES 1 3/8"(front) to 7/8"(back), 1/4" in WALL THICKNESS and 1 1/8" in INTERNAL WIDTH by 2 3/8 in INTERNAL LENGTH.
HINGE IS WORKING AT 100%, SNAPS SHUT & STAYS CLOSED. PIN MEASURES 3 3/8" in LENGTH, 1/4" in WALL THICKNESS and 1 1/4 in WIDTH with 2 PIECE PINBACK. BRACELET & PIN PASS THE TAP TEST(CLUNK), THE HOT WATER TEST(THE SMELL) and THE SIMICHROME TEST(YELLOWYELLOWYELLOW). I MEASURE ALL BRACELETS & JEWELRY with a CALIPER that gives very precise measurements so please keep this in mind. My 2 3/8" is equal to 2 1/2" measured with a ruler or tape measure.
VERY EXCELLENT Vintage Condition, commensurate with age and wear. Please remember that this is 70+ years old and has been previously worn! DO VIEW MY OTHER INTRIGUING Vintage BAKELITE BRACELETS THIS WEEK! The item "HIGHLY CARVED & PIERCED CHERRY AMBER VTG Bakelite Hinged BRACELET PIN BROOCH" is in sale since Saturday, January 12, 2019. This item is in the category "Jewelry & Watches\Vintage & Antique Jewelry\Costume\Bakelite, Vintage Plastics\Bracelets".
The seller is "maur56" and is located in Trenton, New Jersey. This item can be shipped worldwide.


This is a placeholder page for Noel Resendez, which means this person is not currently on this site. We do suggest using the tools below to find Noel Resendez.
You are visiting the placeholder page for Noel Resendez. This page is here because someone used our placeholder utility to look for Noel Resendez. We created this page automatically in hopes Noel Resendez would find it. If you are not Noel Resendez, but are an alumni of Banquete High School, register on this site for free now.


The Intern License (Alternatives 4 and 5) is granted in critical shortage areas or specific site certification plans.
An applicant may be employed as an educator after obtaining a statement of eligibility from the bureau while completing an individualized professional development plan.
May 11 – the NH Board of Education adopted the ACTFL Oral Proficiency Interview (OPI) as a means for candidates establish proficiency in languages.
(4) non-refundable processing fee of $50.00. Make check payable to the STATE OF NEW HAMPSHIRE.
(2) for elementary education, coursework in Mathematics, English, Social Studies, and Science 2.5 GPA.
The school district must appoint a mentor teacher to provide support for the candidate. Eligibility requirements are available from the Bureau.


text:
Scootering classics: Crossing over
23rd July 2018 Features, Show Us Your Scoots
When Paul Douglas decided to build a Lambretta street racer it was only natural that his first love would inspire him…
Any readers who are now in their 50s, no matter how 'Mod' their teenage years, will probably raise a smile at the mention of a Fizzy or more accurately a Yamaha FS 1 E sports moped. Even if their own ride was a 50 Special the chances are that at least one friend would be riding alongside on their Fizzy. It was the combined experience of riding and of being free to go anywhere, without relying on parents or public transport, which drew motorcycling into many of our veins. School friendships enabled us to compare and contrast our chosen transport and endlessly debate their merits when we should have been concentrating on more important things, like exams. If my classmate Malcolm is reading this I'll finally concede that my 50 Special was no match for a Fizzy – at least not until I discovered Pinasco!
The joy of a Fizzy never ends.
"If it's got two wheels I love it," says Paul, which is good news for his employer because he earns a living a motorcycle showroom manager at Team Roberts Triumph in Doncaster. A scooterist since the early 1980s Paul is equally at home on a superbike as he is on a Lambretta, but it was on a little Yamaha that he first felt the adrenaline rush which only two wheels can supply.
Bespoke items produced by K2 Engineering.
"That little Fizzy changed me," admits Paul. "Pretty much all of my adult life had been shaped by those early riding experiences.
"The Fizzy was more than a moped, as until its release mopeds were things that old ladies rode and because they were so dull 16-year-olds were allowed to ride them. Yamaha recognised the gap and created the sports moped. Early versions didn't have to be restricted, they were legal as long as they were under 50cc and could be pedalled. It was only when law-makers woke up to the fun we were having that the 30mph restriction came in."
It's well known that prior to 'the film' scooters were all but extinct in the south of England with only a few diehards keeping the torch burning. It was a different story in the north however. "I'd be riding around on the Fizzy and all the time seeing older lads on scooters," said Paul. "I thought they were cool in a way that motorcycles could never be. Personally I see them as different beasts. If I want to ride at 100mph I'll do it on a sports bike but for sheer style it has to be a scooter." Paul rarely does things by halves and when the time came to say goodbye to the Fizzy it was swapped for a full-on lights and mirrors equipped GS.
Over the years Paul has owned many very tidy scooters. His most recent creation, 'Peaky Blinders', featured on Scootering's cover earlier this year and 1980s icon 'Piss In My Eye Boogie' was in his care for quite some time. When the time came to build his own Lambretta street-racer it was to the Fizzy that he turned for inspiration.
Bring on Kenny
It wasn't just speed that created the Fizzy legend, it was style. Painted in Yamaha's iconic 'speed block' scheme, the Fizzy was equally at home outside the chippy or mixing with its larger siblings outside a biker's cafe. Although the design was used across most of their range it's most associated with the legendary racer Kenny Roberts.
Before going any further it's worth clarifying one point. Paul's employers Team Roberts and Kenny Roberts aren't connected. "Kenny is one of my great sporting heroes," explains Paul and with good reason. The American rider transformed motor racing in more ways than one. Look at any motorcycle racer and you'll see the same stance on cornering, body forward and knee down shifting weight to the front wheel enabling the rear wheel to break contact with the road and slide around the corner. It's the same stance in MotoGP or BSSO and Kenny perfected it,
Having cut his teeth on dirt tracks he was signed by Yamaha USA at the age of 19. Put simply he rode on hard surfaces exactly as he did on the dirt. In a 13-year professional racing career, Roberts won two Grand National Championships, three 500cc world championships including 32 Grand Nationals and 24 Grand Prix road races. If that weren't enough he also won the Daytona 200 three times and the Laguna Seca 200 on six occasions.
Unmistakably Roberts, distinctively Lambretta.
With fame comes influence and Roberts campaigned tirelessly for improved conditions and prize money. It was his declaration of a separate race series in 1979 that finally brought professionalism to the sport and set the scene for Grand Prix motorcycle racing as we know it today.
Grand Prix tribute
There has been more than one attempt to apply motorcycle racing schemes onto scooters over the years — not all of them successful. Paul's successfully transferred the Roberts yellow racer colours onto a Lambretta by taking the spirit of the scheme rather than insisting on a slavish application. Local painter Paul Firth's interpretation is instantly recognisable as a Roberts tribute, but has been executed in a way that suits the Lambretta's distinctive shape.
If the scheme doesn't give it away, the signature will.
Perhaps due to his day job, Paul's quite happy to delegate tasks which can be better handled by experts and the engine on this machine's no exception. "It's a Honda 205 conversion that club mate Chris Swift sourced for me and so far has been trouble free. The suspension's been upgraded to BGM units and I've fitted SIP rims. Those, together with the hydraulic disc have made a large difference to the handling. It's still very much a Lambretta but overall it feels much firmer and controlled to ride than a standard machine"
Paul isn't unique among modern scooterists in spreading his riding across genres but he's perhaps one of the most informed. Call in to Team Roberts and the chances are you'll find one of these two gorgeous street racers in the showroom with Paul ready to talk about their merits just as passionately as latest superbike from Triumph. Some things never change.
MAN & MACHINE
Name: Paul Douglas
Job: Sales manager
Scooter club & town: Rotherham Scooter Club
How and when did you first become interested in scooters: Back in 1979, I think like all young 14-year-olds… Quadrophenia! Following all the lads on scooters who were older with our parkas and suede boots, trying to be in with the crowd. Good days.
First scooter: GP150.
Favourite scooter model: SX200.
Favourite style of custom scooter: Anything that just says time spent on it.
First rally or event: Bridlington.
Favourite rally: Bridlington.
Funniest experience with a scooter: Going out on the scooter, following my mate Hodgy round a corner and not having time to slow down before a hump back bridge… he got both wheels up in the air, then came back down and hit the deck; scooter was all over the place. Hodgy was laughing his head off, a good night out.
What do you like about rallies/ events: Seeing all customs scooters, night life's good but I get sent home early because I'm not particularly good at drinking!
What do you dislike about rallies/ events: Moaners.
What's your favourite Scootering magazine feature: All of it.
Favourite custom/featured scooter of all time: Top Gun.
If you had to recommend one scooter part or item of riding kit what would it be: Best helmet that you can afford.
What's the most useless part you've ever bought for one of your scooters: Stainless steel runner board protectors.
Name of scooter: Marlboro Racer & Team Roberts.
Scooter model: Both 200.
Inspiration for project: I wanted a street racer.
Team Roberts Spec:
Kit: Honda 205.
Crank: Race.
Exhaust: TT Carbon Can.
Dyne done by: Darrell Taylor.
Suspension: BGM Dampers.
Rims: SIP.
Marlboro Spec:
Kit: TS1.
Exhaust: JL.
Engine by: MB.
Dyno done by: Darrell Taylor,
Suspension: Kawasaki Dampers.
Both reliable: Yes, up to now.
Paintwork & murals done by: Paul Firth.
Chrome: Quality Chrome.
What was the hardest part of the project: Getting good fitting bits.
Do you have any advice or tech tips for anyone starting a project: Dry build first.
Is there anyone you wish to thank: Chris Swift, Paul Firth, Darrell Taylor, MB, KBR scooters.
Also Zoe Douglas and Jamie Douglas as it's their inheritance I've just spent!
Paul's daily ride is a GP that once sported Quadrophenia tribute panel. Following a terminal engine breakdown on the way to Bridlington, it was dispatched to be finished in a fictional Team Roberts scheme to create a talking point at the showroom. While the paintwork was being completed by Paul Firth its engine was dispatched to Mark Broadhurst to work his magic, returning equipped with a TS1 225. A very clean and well executed machine it deserves a place in Scootering simply because it's the type of scooter that no longer stands out in the crowd.
Old school repurposed steering dampers.
Think about that for a moment – bespoke seat, Nissin hydraulic front brake, state-of-the-art tuning, updated suspension and a beautifully executed street racer paint scheme. Fifteen, perhaps 10 years ago it would have graced our cover and picked up trophies galore. Taken to a rally in the 1980s it would have seemed like something from science fiction.
That's a very neat everyday ride.
The sad fact is that we've become accustomed to excellence and we take so much for granted. The new season's upon us and there's never been more equipment available to make our scooters more reliable and powerful than ever before. Get out there to rallies large and small, meet friends old and new, but while you're there step back for a moment and take in the machinery around you. We're living in a golden age and just like Paul's daily ride it's worth savouring.
Words: Stan
Photographs: Gary Chapman
Previous Post:Scootering classics: Liquid Cooled – The Norrie Kerr Story
Next Post:Scootering classics: Sculpting of a scooter