It may not have the glamour and appreciation of opportunity of Cannes, the romance of Venice or the boutique cliquishness of Telluride, but for sheer magnitude and scope, the Toronto international cinema celebration( or Tiff, to give it its perkily approachable abbreviation) is hard to beat. Even having cut its programme by 20% this year( about 60 films fewer than previous instalments ), Toronto is a monster of an event.
This means various happenings. The first, and least welcome, of these is queues. Miles of them, snaking around the streets of the city for blockings and be administered by organizations that border on the Kafkaesque. Punters join them automatically, sometimes without knowing what they are waiting for. But the queues are there for a ground, which makes us to the second point: the sheer number of chatter names. The timing of Toronto and its size means that it is an ideal platform on which to test whether a standing claim has the legs to make it a hopeful in the honors race.
Early express suggest that it's going to be another hard-fought engagement in the best actress category, with a affluence of meaty, female-driven narrations. And the crowd-pleasing Battle of the Sexes , the most recent from the Little Miss Sunshine leading duo of Valerie Faris and Jonathan Dayton, is top of the list. Starring Emma Stone as tennis player Billie Jean King, the movie tells the story of the much-publicised 1973 tennis equal between King and ex-champion, and self-proclaimed male-chauvinist boar, Bobby Riggs( Steve Carell, all tragicomic bluster and condescension ). But more than that it's a love story, in which King, hopelessly smitten with hairdresser Marilyn( Andrea Riseborough ), was necessary to words with her own sexuality. Stone is terrific, throwing King a steely sweetness and a disarming vulnerability. And although some of the overt antediluvian sexism from the commentators sucked audible gasp from the gathering, the topics- equal money and equal opportunities for women, LGBT acceptance in play- persist depressingly timely.
Another powerhouse female leading comes from Jessica Chastain, playing the eponymous central character in Aaron Sorkin's directorial introduction, Molly's Game . This is pretty much the archetypal Sorkin project- a slick firework parade of showy dialogue and jostling ideas and a prime persona with a humor that Chastain holds like a flick knife. Based on a real-life character, Molly is a former Olympic-standard skier turned hostess of unlicensed, high-stakes poker games, who experiences herself at the center of an FBI investigation. While Sorkin panders in a few too many self-congratulatory segues and prosper, as long as Chastain is on screen- and she's rarely off- the movie has a crackling force and propulsive drive.
The world of sport was a repetition theme at this year's gala, which opened with more tennis squabbling courtesy of the witty Borg vs McEnroe . Perhaps more of a long shot in the gifts posts, but one of the most wonderful tickets of the festival, I, Tonya stars Margot Robbie as shamed American chassis skater Tonya Harding. The latest film from Craig Gillespie( Lars and the Real Girl ), this is a deftly handled juggling ordinance of a movie that balances the conflicting accountings- and the barefaced lies- from the key doubts in the attack on competitive skater Nancy Kerrigan. Armed with a bad perm and a offering for curse, Tonya is a gift of a character for Robbie, who attacks the specific characteristics with the same forceful, gutsy, take-no-prisoners attitude that Tonya brought to her triple axel. Gillespie, meanwhile, plucks off a touchy compounding of mining the material for slapstick- and it is very funny- without balk away from the darker elements of Harding's story: the abuse, the discrimination and the toxic father( a gorgeously poisonous Allison Janney ).
Another peach of a conduct comes from one of various strong British films that proved at the celebration. In Film Stars Don't Die in Liverpool , Annette Bening plays Oscar-winning Hollywood star Gloria Grahame at the end of their own lives when she started on a relationship with a young performer from Liverpool( an impressive, and unexpectedly buff, Jamie Bell ). Bening faces competitor on screen from make designing that goes all out to capture the real fright of British provincial interior design of the 1970 s, but even wallpaper that bellows tortured florals is no pair for her. She brilliantly captures the appeal of a virtuoso whose most enduring and consuming capacity is herself.
Of the other British honors competitors, a standout is necessary Joe Wright's take on the events circumventing the Dunkirk removals of 1940. Darkest Hour stars Gary Oldman as Winston Churchill, newly appointed as prime minister and grappling with the decision of whether to negotiate terms with the Germans or whether to hold firm and perhaps stand disastrous loss among the troops massed on the beaches in France. This is a film in which words, rather than artilleries, are the weapons of selection and Oldman, while not an exact coincide for the jowly physicality of Churchill, captures his slurred but whisking style of speech brilliantly.
Oldman's blustering, booze-sodden action, together with Wright's visually playful attitude, is necessary that even without a single hit of troops on the beaches the film parcels in as much breathless drama as Christopher Nolan's Dunkirk . It also has the bonus of a strand of flippant humour; all-important, given how many situations involve pompous privileged males in suits propping forth in stuffy, wood-panelled rooms.
The extensive showcase of British cinema premiering at the gala also includes Armando Iannucci's abrasively entertaining The Death of Stalin ; Clio Barnard's savage urban lineage drama Dark River and the astonishing aspect introduction from Michael Pearce, Beast .
Iannucci's picture is a generally acerbic and contemptuous look at the jostling power play of the inner circles of government. In this case, however, the government is that of the USSR, thrown into tangle by the death of Stalin. There are many intellects to watch this, but the main one is Simon Russell Beale in the responsibilities of the Lavrentiy Beria. I can't think of a conduct more saturated with gleeful malice , nor one I have enjoyed more this festival.
Dark River is a paint that deals with the bequest of defamation, with Barnard's trademark psychological ability and sense, to devastating effect. And Beast channels an earthy, seductive threat into a Sleeping With the Enemy proposition, set against the conservative backdrop of Jersey. It likewise showcases a formidable aptitude, in the forms of compelling whiz Jessie Buckley.
But of all the movies in this year's celebration, my favourite is another sending introduction, from actor Greta Gerwig. Lady Bird , starring Saoirse Ronan as a young woman coming of age in north California, is a exhilaration. A dexterous, agile slapstick and a utterly persuasion, fleshed-out persona examine, this drawing announces Gerwig as an important ability behind the camera as well as in front. Christine, aka Lady Bird( Ronan ), is a composite, maddeningly pretentious, utterly endearing reputation. Like almost everyone else in Toronto, I descended wholly in love with her.


It's about that feeling. The feeling when you're stuck and not getting anywhere. No one understands you. That feeling. It's more than frustration. It is a place where creativity slowly lies down and dies.
Therefore, Untz Untz exists. A sanctuary for creativity. All those sayings that come and go. With Untz Untz they have a home.
Look through some of what we have amused ourselves with since the start in 2010.
Untz Untz is brought to you with Jenny Karlsson.
The world's first earth-revolving campaign.
An absolute favorite, a collaboration between YouTube and Chanel.
Some of the best Untz Untz posters (all available on Untz Untz's Facebook page).


The LifeLine Animal Project was established in 2002 by Rebecca Guinn with the mission to end the euthanasia of healthy and treatable dogs and cats in shelters across metro Atlanta. They work towards this mission through several programs and events, and as of 2013, LifeLine is the managing organization of both the Fulton County Animal Services as well as the DeKalb County Services shelter.
Back in 2002 the founder of LifeLine, Rebecca Guinn, at the time a litigator, discovered a stray dog. She took this healthy dog to the local shelter there in DeKalb and was struck by how many dogs were there. But when she returned to the shelter a short while later to check on that dog she had dropped off, she was horrified to find the shelter was empty. Almost all the animals had been euthanized in that short period and she decided right then that she had to do something about it. Soon after, she left her job and started this nonprofit. In the beginning, she developed an online database for the animals in the shelters, to create an easier model for adoption here in Atlanta and LifeLine only grew from there. Guinn went on to establish her first shelter in Avondale Estates, DeKalb where she focused on animals in need, such as those who were sick or abused who were the hardest for other shelters to care for and who were the most at risk of being euthanized.
Cooper, on a weekend adventure as part of LifeLine's Weekend Warrior program For all the amazing things she accomplished with this shelter, she realized that the best way that she could end euthanasia in shelters was to get into those shelters. In 2012, LifeLine put in for the contracts to both the Fulton County Animal Services shelter and the Dekalb County Animal Services shelter, and in 2013 they were awarded both of those contracts. Getting both contracts at once was an amazing opportunity to effect change yet at the same time, it was a significant challenge, but one that LifeLine took to with gusto. Since taking over these contracts, they have increased the Lifesaving rates in these shelters dramatically. Prior to their involvement, Fulton county had a Lifesaving rate of 39% and DeKalb County had a Lifesaving rate of 61%. Now they both range from 85% to 89% an increase that is a resounding success for LifeLine, but it is still not enough for LifeLine. LifeLine's goal is to eliminate euthanasia outside of extreme cases so their work is still very much alive.
Now that they are doing all that they can in the shelter, LifeLine's work has expanded even beyond the shelter. A key element to LifeLine's mission is to put the pets first, to ensure that these animals are happy and healthy in order to keep them from ever coming to the shelters in the first place. One important way they are accomplishing this is through low-cost veterinary services such as spay and neuter, vaccinations, flea treatment, and more. They have two LifeLine Spay and Neuter Clinics (one in Avondale Estates and one in College Park) at which they offer low-cost and free spaying and neutering to help reduce the amount of homeless animals. Furthermore, they are even in the process of building a community center which will offer not only low-cost or free spaying and neutering services, but even low or zero cost veterinary services to ensure that these animals are given the best care. This center will be open to anyone, regardless of income, as the health of the pets comes first to LifeLine.
Additionally, LifeLine has been working closely with Pets for Life, a program initiated by the Humane Society. This program works to provide pet supplies, spay and neuter services, veterinary care, and more door-to-door in areas that are underserved by pet supply stores and veterinary clinics. Currently this program is still in its infancy, and LifeLine is working hard to scale the service and hopes to expand it to ensure every pet in underserved areas can get access to these services.
Ginger, one of LifeLine's many foster dogs Furthermore, through Pets for Life, LifeLine host four big events a year known as their Healthy Pets Events. There are two in Fulton and two in DeKalb, each county has one in the spring (April and May) and one in the fall (October and November). During the Healthy Pets Events they host a four hour clinic during which people can come with their pets and LifeLine offers free vaccinations, free veterinary services, free spay and neuter vouchers, pet supplies, as well as food (for both people and pets alike). These events are open to any and everyone, LifeLine is truly dedicated to helping every pet they can.
Beyond simply offering their services in order to keep animals out of the shelters, LifeLine works to spread the word about the importance of spaying and neutering pet and to stop backyard breeding. LifeLine is working to advocate without judgment and seeks to advocate for these animals without disparaging those who are dealing with them, instead they want to work with them for the benefit of the animals, to work alongside them for the betterment of these animals' lives and to move towards the future LifeLine envisions.
But overall, the biggest way that LifeLine is working to eliminate euthanasia is through their collaborative efforts with their amazing partners such as the Humane Society of Atlanta, Best Friends Animal Society, and more. It is with their support that LifeLine has made, and continues to make, such incredible strides towards their goal of eliminating euthanasia in Atlanta's shelters.
One such partner that is incredibly important is the Rescue Dog Olympics. LifeLine's goals run parallel to the Rescue Dog Olympics, as everything that LifeLine does is for the benefit of these pets. But even more important is that the Rescue Dog Olympics provide an amazing avenue through which LifeLine can spread the word, advocate for their mission, and to make inroads with the community. It is this deep connection with the community that serves as LifeLine's lifeblood, their established network of rescue partners who are there for LifeLine during the massive influx of dogs, cats, or more due to hoarding cases, and other extreme events that grants them the power to have improved the lifesaving rate in Atlanta and that will continue to support them on their mission. This year's Rescue Dog Olympics is going to be on Sunday, March 10, 2019, and will be held in Piedmont Park, Atlanta, so pre register and drop on by!
LifeLine relies on its volunteers, donors, and of course those who adopt. Visit the LifeLine Animal Project website for information on how to donate, volunteer, adopt, and more to help out or find your new best friend.


text:
\section{Introduction}

Of the three principal baryonic components of any galaxy -- stars, gas,
and dust -- the distribution of dust is the least understood.  The
radial density
distribution of the stellar component in disk galaxies falls off
exponentially with a scale length ranging from $\sim$1~-~10~kpc
(de Jong 1996a,1996c) out to an
abrupt radial cutoff (van der Kruit and Searle
1981a, 1981b, 1982a, 1982b).  The radial density distribution of neutral hydrogen
is flat (e.g. Shaya and Federman 1987) out to a radial cutoff, while
that of
molecular gas is generally
exponentially decreasing (e.g. Young and Scoville 1991) even though
there is evidence for the presence of cold molecular gas at large
galactic radii (e.g. Lequeux {\it et al.\ } 1993; Fich {\it et al.\ } 1989; Wouterloot {\it et al.\ } 1990).
These various distributions have been used to study the
formation of disks (cf. Fall \& Efstathiou 1980; Lin \& Pringle 1987), star formation in disks (Kennicutt 1989),
and the relation between the neutral hydrogen fraction and the ionizing intergalactic radiation field
(Maloney 1993).  Does dust
trace the stellar or gaseous components (either the atomic or molecular
phase)?  The resolution of this question may yield insight into
past star formation in galactic disks and into the energetics and transport
of the interstellar medium throughout disks.  The goal of this study is to
infer the average radial and angular distribution of dust at large radii
in galaxies, by measuring the 100$\mu$m emission from
ensembles of galaxies.

Existing studies of
dust in galaxies rely on one of two physical phenonemon:  (1)  the
extinction of light by dust grains (e.g. Zaritsky 1994; Block {\it et al.\ } 1994; Peletier {\it et al.\ } 1995; de Jong 1996b); and (2)  the emission of FIR/mm light by dust grains (e.g. Rice {\it et al.\ } 1988; Bothun \& Rogers 1992; Andreani \& Franceschini 1996;
Odenwald, Newmark \& Smoot 1996).  The application of either approach
becomes increasingly difficult at larger radii.  By measuring the
extinction of background galaxies observed through the halos of
two large, nearby spirals, Zaritsky (1994)
presented preliminary evidence of dust at radii of
$\sim$60~kpc.  Studies of the far-IR emission from galaxies have focused on dust
within the optically luminous disks of nearby galaxies of large
angular extent (Rice et
al. 1988; Bothun, Lonsdale, Rice 1989; Bothun \& Rogers 1992; Rice
1993).  Bothun and Rogers (1992) detected 100$\mu$m emission
out to approximately 30~kpc in 6 of the 28 galaxies in their sample.
However, the signal-to-noise is rather low in these outer regions, and there
is limited spatial information.  Reliable, general constraints on
the distribution of dust beyond $\sim$15~kpc are scarce.

We strive for sensitivity by coadding the
100$\mu$m images
of 115 galaxies drawn
from the IRAS Sky Survey Atlas (ISSA; Wheelock {\it et al.\ } 1994) to measure the radial extent,
profile, and azimuthal distribution of the thermal dust emission.  We
choose to work with the longest wavelength IRAS images because we are interested in the
distribution of dust at large radii, which is most likely cold
($\mathrel{\spose{\lower 3pt\hbox{$\mathchar"218$} 30K$) and
therefore has peak emission at $\lambda \mathrel{\spose{\lower 3pt\hbox{$\mathchar"218$} 100\mu$m.
In $\S$2, we discuss the selection
criteria for the sample and control galaxies, and describe our
algorithm. In $\S$3, we present the results obtained from the two samples.
Finally, in $\S$4, we model the 100$\mu$m emission, and present
a simple model which constrains the dust distribution.

\section{The Data}

\subsection{Sample Selection}

\begin{figure}
\epsscale{1.0}
\plotfiddle{fig1.pp.ps}{4in}{0}{70}{70}{-210}{-90}
\caption{A $\sim 20^{\circ} \times 20^{\circ}$ section of the
ISSA Atlas near $(\alpha,~\delta) = (1^{h}20^{m},~0^{\circ})$ or
equivalently $({\it l},{\it b}) = (139.5^{\circ},~-61.6^{\circ})$.
The filamentary features of large angular extent are due to Galactic
cirrus, while the numerous small higher surface brightness knots are
predominantly galaxies.\label{f1}}
\end{figure}

Our measurement of the emission from cold dust in galaxies is
based on the combination of 100$\mu$m ISSA images (Wheelock {\it et al.\ }
1994) and basic galactic data from the Third Reference Catalog of Bright
Galaxies (RC3; de Vaucouleurs et
al. 1991).  We limit
our study to Galactic latitudes $b \mathrel{\spose{\lower 3pt\hbox{$\mathchar"218$} 15^\circ$ and $b \mathrel{\spose{\lower 3pt\hbox{$\mathchar"218$} -40^\circ$ to minimize Galactic cirrus
contamination and select candidates from the RC3 based solely on their coordinate
positions, regardless of other galactic properties such as morphology.
Figure~\ref{f1}~shows a
$\sim20^\circ \times 20^\circ$
section of the 100$\mu$m Atlas near ($\alpha$,$\delta$) = (1$^h$20$^m$, 0$^\circ$) or equivalently
(${\it l},{\it b}$) = (139.5$^\circ$, $-$61.6$^\circ$).  The images have
1.5$^{\prime}$ pixels.
The filamentary features of large angular extent
are due to Galactic cirrus (Low {\it et al.\ } 1984).  The numerous small, high surface brightness knots are
predominantly galaxies and are typically comparable in size to the point spread function
of the survey (FWHM $\simeq~5^{\prime}$; ISSA Explanatory Supplement).

The most serious difficulty faced by this study is the irregular structure of the Galactic foreground emission.
As illustrated in Figure~\ref{f1}, the contamination can be high even at high
galactic latitude.  To ensure that the final sample of galaxies do not
have close companions and that they lie in quiescent regions of the foreground
sky, we identify each candidate on the ISSA images using
the RC3 coordinates and
a gnomic coordinate projection centered on the central coordinates of our
35$^\circ$ survey images, and apply the following criteria:

\noindent  ${\it (1)~~Centering~Convergence:}$  The galaxies' 100$\mu$m luminosity
centroids are calculated using the IRAF CENTER
routine\footnote{IRAF is distributed by the
National Optical Astronomical Observatories, which are operated
by AURA, Inc., under contract to the NSF.}.
We reject galaxies with 100$\mu$m centroids that have internal
uncertainties $>$0.45$^{\prime}$ in either
x or y ($>$ 1/3 of a pixel), or that have 100$\mu$m centroids that differ by more than
2.25$^{\prime}$ ($\sim0.5\times$FWHM of a point source)
from the projected coordinates.  Typically, galaxies fail these
criteria if they have low signal-to-noise, a close companion, or lie in regions of
high cirrus contamination.  About 90$\%$ of the original 23660 possible target
galaxies are rejected due to this criteria.

\noindent  ${\it (2)~~ Photometric~Convergence:}$  We perform aperture photometry on the remaining galaxy candidates using the
IRAF PHOT routine and apertures with radii
from 1.5$^{\prime}$ to 10.5$^{\prime}$ spaced by 1.5$^{\prime}$. We reject any galaxy whose magnitude does not converge
on the grounds that the local background must be strongly affected by
cirrus emission.  This step excludes $\sim6\%$ of the remaining targets.

\noindent ${\it (3)~~Image~Edge~and~Bad~Pixel~Contamination:}$
Galaxies within 52.5$^{\prime}$ (a distance equal to the region of the
extracted subimage used in the analysis) of the image edge are
rejected.  In addition, the process of mosaicing smaller images to
produce the $\sim30^{\circ}~\times~30^{\circ}$ ISSA images can create
streaks of bad pixels at the interface of the sub-images.  Any
galaxies falling in regions of these bad pixel streaks are rejected.
Because both the shape of the final mosaic images and the initial
sub-images vary from image to image, this step is done interactively and excludes $\sim17\%$ of the remaining galaxies.

\noindent  ${\it (4)~~Multiple~Identifications:}$  Any 100$\mu$m
source that was associated with multiple optical sources was rejected;
excluding $\sim9\%$ of the remaining galaxies.

\noindent  ${\it (5)~~Close~Companion~Contamination:}$
To avoid contamination from
close companion galaxies, we reject any galaxy with a cataloged
companion within 30$^{\prime}$
projected separation.  This cut excludes
$\sim20\%$ of the remaining targets.

\noindent  ${\it (6)~~Visual~Inspection:}$  To ensure
that the final galaxy sample is not contaminated by either strong
cirrus or close companions not listed in the RC3, we visually inspected
each image.  Interactively,
we only removed 3$\%$ of the remaining galaxies.  Overall, 95$\%$ of
the original galaxies are rejected due to the above cuts.

This procedure yields a heterogeneous set of isolated galaxies, which span a
wide range of sizes, distances, luminosities, and inclinations.  For the
addition of galaxy images to be physically meaningful, we must
normalize their apparent angular scales and brightness using
their isophotal diameters and their central surface brightnesses.  In
defining the final samples, we want to maximize the number of galaxies to
increase the sensitivity yet minimize the range of isophotal diameters and central surface
brightness to avoid large scaling factors that greatly magnify
the point spread function, PSF, (which could mask an otherwise
resolvable detection) and decrease the signal-to-noise ratio.
Therefore, we
impose two conditions.  First, the isophotal diameters of galaxies in
any particular sample cannot be scaled by more than a
factor of three.  We bin the samples into three groups according to $D_{25}$:  $2.5^{\prime} - 5^{\prime}$, $5^{\prime} - 10^{\prime}$, and
$10^{\prime} - 30^{\prime}$.  Second, the galaxies must be within a
limited range of intrinsic
luminosities.  We include those
galaxies in the $2.5^{\prime} - 5^{\prime}$ and $5^{\prime} - 10^{\prime}$ samples that
have $-18 > M_B > -23$ (H$_{0} = 75$~km/s/Mpc in all calculations).  The
galaxies in the $10^{\prime} - 30^{\prime}$ sample are sufficiently nearby that calculating luminosities using
recessional velocities, $V_{rad}$, is not accurate ($\langle V_{rad} \rangle =
748$~km/s), so no luminosity cuts are made.

\begin{figure}
\epsscale{1.0}
\plotfiddle{fig2.ps}{4in}{0}{70}{70}{-210}{-70}
\caption{The distributions of recessional velocities and R$_{25}$
for the $10^{\prime} - 30^{\prime}$ sample of 24 galaxies.\label{f2}}
\end{figure}

\begin{figure}
\epsscale{1.0}
\plotfiddle{fig3.ps}{4in}{0}{70}{70}{-210}{-70}
\caption{The distributions of recessional velocities, R$_{25}$,
and M$_{B}$ for the $5^{\prime} - 10^{\prime}$ sample of 91 galaxies.\label{f3}}
\end{figure}

\begin{figure}
\epsscale{1.0}
\plotfiddle{fig4.ps}{4in}{0}{70}{70}{-210}{-75}
\caption{The distributions of recessional velocities, R$_{25}$,
and M$_{B}$ for the $2.5^{\prime} - 5^{\prime}$ sample of 184 galaxies.\label{f4}}
\end{figure}

\begin{figure}
\epsscale{1.0}
\plotfiddle{fig5.pp.ps}{4in}{-90}{70}{70}{-290}{390}
\caption{The distribution of galaxy type, as listed in the RC3,
for all three samples of galaxies and the control galaxies.\label{f5}}
\end{figure}

\begin{deluxetable}{lcccccc}
\footnotesize
\tablewidth{0pt}
\tablecaption{Sample Properties \label{t1}}
\tablehead{
Sample & \colhead{Number} & \colhead{D$_{25}$} & \colhead{V$_{rad}$ (km/s)} & \colhead{$\langle$V$_{rad} \rangle$
(km/s)} & \colhead{M$_{B}$ (mag)} & \colhead{$\langle$R$_{25}\rangle$
(kpc)}
}
\startdata
$10^{\prime} - 30^{\prime}$ & $24$ & $10^{\prime} - 30^{\prime}$ & $0 - 1600$ & $750$ &
\nodata & $18.9$\nl
$5^{\prime} - 10^{\prime}$ & $91$ & $5^{\prime} - 10^{\prime}$ & $500 - 3300$ & $1500$ &
$-18$ to $-23$ & $18.1$\nl
$2.5^{\prime} - 5^{\prime}$ & $184$ & $2.5^{\prime} - 5^{\prime}$ & $700 - 6800$ &
$2100$ & $-18$ to $-23$ & $13.6$\nl
Control Galaxies & $200$ & $0^{\prime} - 1.5^{\prime}$ & $1000 - 16000$ & $5800$ & $-18$
to $-23$ & \nodata\nl
Control Stars & $30$ & \nodata & \nodata & \nodata & \nodata & \nodata\nl
\enddata
\end{deluxetable}

The final samples
consist of 24 galaxies in the $10^{\prime} - 30^{\prime}$ sample, 91
galaxies in the $5^{\prime} - 10^{\prime}$ sample, and 184 galaxies in the $2.5^{\prime} - 5^{\prime}$ sample.  The distributions of recessional velocities,
R$_{25}$, and M$_{B}$ for each sample, if available, are shown in
Figures~\ref{f2},~\ref{f3},~\ref{f4}.  A
summary of the mean properties of each sample is given in Table~\ref{t1}.
Although no selection criteria were imposed regarding galaxy type, the
samples are predominantly galaxies classified as
type Sd to Sa in the RC3, as shown in Figure~\ref{f5}.  This is an
indirect result of selecting galaxies from the 100$\mu$m images, a
spectral regime where emission from dusty late-type galaxies dominates
over the relatively dust-free early-type galaxies.  Notice that the
galaxies in the $10^{\prime}~-~30^{\prime}$ and $5^{\prime}~-~10^{\prime}$ samples
appear to contain nearly identical galaxies because they both have
$\langle R_{25} \rangle \sim 18.5$~kpc, while the $2.5^{\prime}~-~5^{\prime}$ sample
appears to be dominated by galaxies that are physically smaller,
$\langle R_{25} \rangle \sim 13.5$~kpc.
Finally, as we discuss below, we take care to select a control sample with the same
quantitative criteria as used to select the original samples.

\subsection{Coadded Images and the Point Spread Function}

The exact procedure we use to prepare the galaxy images to be coadded consists of
the following steps:

\noindent (1) we extract a subimage of $121.5^{\prime} \times
121.5^{\prime}$ (81 pixels)
centered on each galaxy using the
100$\mu$m galaxy centroid;

\noindent (2) this subimage
is rotated and scaled using IRAF's IMLINTRAN routine and the optical
position angle and D$_{25}$ from the RC3, while
conserving total flux;

\noindent (3) we subtract
a mean sky value measured in an annulus defined by $30^{\prime} < R < 52.5^{\prime}$
, where R is the radius from the target galaxy; and

\noindent (4) we normalize the flux, as measured by our aperture photometry, so that the galaxy's central
surface brightness is equal to unity.

\noindent Upon completion,
the resulting images of each galaxy are combined into a mean and median image,
applying $10\sigma$ clipping to remove spurious pixels.
The outer border (width = 10 pixels) of the resulting co-added image is fit by a plane
to remove any large scale sky variations.  The image is then rebinned into polar
coordinates, which allows a straightforward comparision of the radial extent
of the 100$\mu$m emission as a function of polar angle (e.g. Fig 7).  Finally, the sky is resubtracted (always a small subtraction, $<
1\%$) and the central surface brightness is renormalized (always a
small division factor, resulting in $< 1\%$ effect). The
result of this procedure is an image in polar coordinates that
is the sum of 184 galaxies in the $2.5^{\prime} - 5^{\prime}$ sample, 91 galaxies in
the $5^{\prime} - 10^{\prime}$ sample, and 24 galaxies in the $10^{\prime} - 30^{\prime}$ sample from
which we measure the shape and extent of
the 100$\mu$m emission.

We do not attempt any correction for galaxy inclination angle.
For all but the most nearby, face-on galaxies, the 5$^{\prime}$ PSF of
the ISSA images equals or exceeds the galaxies' minor axes.  However,
the major difficulty with any attempt at deprojection is the complex
background component that cannot be removed on a galaxy-by-galaxy
basis.  The other option to address this issue, exclusion of lower
inclination galaxies, is also not tenable.  This option substantially
decreases the sample size and our ability to detect emission at large
radii.  Therefore, we have chosen to apply no inclination correction,
but only present quantitative results from data taken along the major
axis of the final summed image, which is least affected by inclination.

Most, if not all, of the 100$\mu$m emission from galaxies in the
samples are dominated by emission from the unresolved or marginally
resolved inner portions of the disks.  Consequently, our ability to
detect extended 100$\mu$m emission is highly dependent on the
determination of an accurate 100$\mu$m point spread function.  At a
distance of 25
Mpc, $\langle$D$_{25} \rangle$
corresponds to 5$^{\prime}$.  The IRAS 100$\mu$m PSF is
$\sim$5$^{\prime}$ on the longest side, but is asymmetric and varies
spatially across the images because of survey coverages and thus, is too complicated to model. We
will rely on an empirical determination from two independent sets of
unresolved sources.

\begin{figure}
\epsscale{1.0}
\plotfiddle{fig6.pp.ps}{4in}{0}{70}{70}{-210}{-70}
\caption{The distributions of recessional velocities, R$_{25}$,
and M$_{B}$ for the control sample of 200 galaxies.\label{f6}}
\end{figure}

To determine the point spread function in an empirical manner that is
entirely consistent with the collection and analysis of our sample, we select two independent sets of unresolved
sources: stars detected in all four bands in the IRAS Faint Source Catalog; and compact
galaxies ($D_{25} \leq 1.5$$^{\prime}$) from the RC3 catalog.  As long
as stars do not have extended structure (such as debris disks or
envelopes) then they are
truly point sources, and so, apparently an ideal control set to
determine the PSF empirically.  Such extended structure is
characterized by an IR excess, and therefore we select stars with
F$_{12}~>~$F$_{60}$, where F$_{12}$ and F$_{60}$ are the fluxes at
12$\mu$m and 60$\mu$m, respectively.  Unfortunately, there are too few stars (30 that survived our selection
criteria) to compare to the more numerous $2.5^{\prime}~-~5^{\prime}$ and $5^{\prime}~-~10^{\prime}$
samples, and the stars
have a much higher central surface brightness than the galaxies, which
may be an issue with detector hysteresis.  However, because the
$10^{\prime}~-~30^{\prime}$ sample is few in number (N$_{10^{\prime}-30^{\prime}}$
= 24) and those galaxies in the sample are bright, we use the stars
to determine the PSF to use for comparison to this sample.  The
compact galaxies are generally
distant ($\langle$V$_{rad}\rangle$ = 5789 km/s) and unresolved ($D_{25} \leq 1.5^{\prime}$).
These control galaxies are much more numerous ($N_{con} =
200$) than the stars, and have brightness characteristics that are
very well matched to the two sets of sample galaxies, $2.5^{^{\prime}}~-~5^{^{\prime}}$ and
$5^{\prime}~-~10^{\prime}$, to which they are compared.  Figure~\ref{f6} shows the
distribution of recessional velocities, $R_{25}$, and $M_B$ for the
control galaxies.  As is the case for the sample galaxies, the control galaxies
are predominantly of types Sc and earlier (see Figure~\ref{f5}).  This set of control
objects results in a conservative estimate of the
PSF because the dust emission from these galaxies is not necessarily unresolved.  See Table~\ref{t1}
for a summary of the mean properties of the two control samples.

We calculate
the PSF using these two control samples and Monte Carlo techniques
to reproduce the range of spatial rescalings and rotations applied to the data.
Our procedure includes:

\noindent (1)  the extraction of a $121.5^{\prime} \times 121.5^{\prime}$
control galaxy sub-image, randomly selected from the complete control
set;

\noindent (2)  the control sub-image is spatially rescaled and rotated
using parameters drawn from a corresponding sample galaxy;

\noindent (3)  the control galaxy is sky-subtracted and
normalized so that its central
surface brightness equals unity, as is done for the sample galaxies.

\noindent These steps are repeated until the number of randomly selected control
galaxies equals the number of sample galaxies.
The control objects are then
coadded using the same algorithm as outlined previously for the sample
galaxies to produce an image of the PSF.  For the $2.5^{\prime} - 5^{\prime}$ and $5^{\prime} - 10^{\prime}$
samples, we repeat this procedure 20
times to get a mean representation of the point spread function and a
measurement of the
uncertainty in the mean PSF.  For the $10^{\prime} - 30^{\prime}$ sample, the number of control stars is
comparable to the number of sample galaxies and thus we only repeat
the above Monte Carlo procedure 10 times to derive a corresponding mean PSF.

\section{Results}

\begin{figure}
\epsscale{1.0}
\plotfiddle{fig7.pp.ps}{4in}{-90}{85}{85}{-400}{465}
\caption{Residual images for the $10^{\prime} -
30^{\prime}$ sample, before $({\it left~panel})$ and after $({\it
right~panel})$ rebinning into polar coordinates.  The left panel image is $\sim 45^{\prime} \times 45^{\prime}$.
The residual is determined by calculating the mean image of the 10
Monte Carlo realizations of the control PSF and subtracting the mean
PSF from the coadded sample of galaxies image.  Lighter shades
correspond to higher flux.  100$\mu$m emission is visible to a radius
of $\sim$1.1R$_{25} \simeq 21$~kpc and is most extended along the major
axis of the disk, demonstrating that 100$\mu$m emitting dust is flattened
into a disk.\label{f7}}
\end{figure}

Any 100$\mu$m flux in excess of that expected from a point source is a
direct detection of extended emission from galaxies.  To determine if
excess emission exists, we construct residual images by subtracting
the PSF image from the coadded sample image.  The residual image for
the $10^{\prime} - 30^{\prime}$ sample is presented in Figure~\ref{f7}, where the
left hand and right hand panels are the residual images before and
after rebinning into polar coordinates, respectively.  The residual image was produced by combining the sample galaxy
images using a median filter.  The right hand panel shows
100$\mu$m emission that is easily visible to a
radius of $\sim$~1.1~R$_{25}~\simeq$~21~kpc.  Also, both panels illustrate that the residual emission is most extended along
the optical major axis of the
disk, thus indicating that the dust responsible for the 100$\mu$m
emission is flattened into a disk.

\begin{deluxetable}{lcc}
\tablewidth{0pt}
\tablecaption{100$\mu$m Emission Detections \label{t2}}
\tablehead{
\colhead{Sample} & \multicolumn{2}{c}{100$\mu$m Emission
Detection}\nl
\nl
\colhead{} & \colhead{2$\sigma$ Detection} & \colhead{1$\sigma$ Detection}
}
\tablecolumns{3}
\startdata
10$^{\prime}$ - 30$^{\prime}$ & 1.1R$_{25}$ & 1.2R$_{25}$\nl
& 21~kpc & 23~kpc\nl
\nl
5$^{\prime}$ - 10$^{\prime}$ & 1.5R$_{25}$ & 1.8R$_{25}$\nl
& 27~kpc & 33~kpc\nl
\nl
$2.5^{\prime} - 5^{\prime}$ & \multicolumn{2}{c}{no emission detected}\nl
\enddata
\end{deluxetable}

\begin{figure}
\epsscale{1.0}
\plotfiddle{fig8.ps}{4in}{-90}{85}{85}{-345}{360}
\caption{The surface brightness profile (averaged over
$0^{\circ} \leq \theta \leq 22.5^{\circ}$, where $\theta$ is the azimuthal angle such that 0$^{\circ}$
is along the disk major axis) for the $10^{\prime} - 30^{\prime}$ sample $({\it
left~panel})$, the $5^{\prime} - 10^{\prime}$ sample $({\it middle~panel})$, and the
$2.5^{\prime} - 5^{\prime}$ sample $({\it right~panel})$.  The mean PSF has been subtracted from the coadded sample galaxies and also
from each individual Monte Carlo realization of the control.  The
scatter of the various realizations of the control residuals are indicative of
the uncertainties and any emission above this scatter is a significant detection.  Extended 100$\mu$m emission is seen to radii of
1.1R$_{25} \sim 21$~kpc for the $10^{\prime} - 30^{\prime}$ sample and 1.5R$_{25} \sim
27$~kpc for the $5^{\prime} - 10^{\prime}$ sample at the $2\sigma$ level.\label{f8}}
\end{figure}

The radial distribution of the residual 100$\mu$m emission (averaged over $0^{\circ} \leq |\theta| \leq
22.5^{\circ}$, where $\theta$ is the angle such that
0$^{\circ}$ is along the disk major axis) for all three samples is shown in Figure~\ref{f8}.  The
mean PSF has been subtracted from the coadded
sample galaxies (combined using a median filter) and also, for comparision, from each individual Monte Carlo realization
of the control.  Uncertainties in the residual surface brightness
profile are calculated from the rms scatter of the various Monte Carlo realizations of the control
samples.  At the
$2\sigma$ level, 100$\mu$m emission extends to a radius of 1.1R$_{25}
\simeq$ 21~kpc for the $10^{\prime}~-~30^{\prime}$ sample and
to 1.2R$_{25} \simeq$ 23~kpc at the $1\sigma$ level (Fig~\ref{f8}, left panel).  For the $5^{\prime} - 10^{\prime}$ sample, residual 100$\mu$m
extended emission is detected to a radius of 1.5R$_{25} \simeq$ 27~kpc at the
2$\sigma$ level and to 1.8R$_{25} \simeq$ 33~kpc at the $1\sigma$
level (Fig~\ref{f8}, middle panel).  The $2.5^{\prime} - 5^{\prime}$ sample
(Fig~\ref{f8}, right panel) shows no significant extended emission at any
radii.  This null detection is consistent with our two previous
detections because the apparent angular
size of the 100$\mu$m detection in the two nearby samples is not resolvable at the mean distance
of the $2.5^{\prime} - 5^{\prime}$ sample and thus
serves as a check on our method, demonstrating that a spurious
detection is not produced by the method.  These results are summarized
in Table~\ref{t2}.  Combination using an average filter produces
virtually identical results (at the 2$\sigma$ level:  1.1R$_{25}
\simeq$ 21~kpc for the $10^{\prime} - 30^{\prime}$ sample and 1.8R$_{25} \simeq$
33~kpc for the $5^{\prime} - 10^{\prime}$ sample) and therefore are not shown explicitly.
Because the results are the same using either the average or median
combination, we are assured that these
detections are not due to one (or a few) dominant galaxies.  Rather,
extended 100$\mu$m emission is a typical feature of disk galaxies.

\section{Discussion}

We now investigate the
distribution of the 100$\mu$m emission in more detail and attempt to
constrain the distribution of dust.  First, we
examine the radial shape of the far-IR surface brightness profile and
compare it to that of the underlying stellar component.  Second, we use a simple model to convert the surface brightness
profile to a dust mass profile.  Finally, we briefly
discuss the implications of our derived dust mass distribution.

\subsection{100$\mu$m Surface Brightness Profile}

We have detected 100$\mu$m emission at radii of 21 kpc
for the $10^{\prime} - 30^{\prime}$ sample and 27 kpc for the $5^{\prime} -
10^{\prime}$ sample at the 2$\sigma$ level, but
what is the shape of that surface brightness profile?
Although the resolution of our data is coarse (HWHM$_{10^{\prime}-30^{\prime}}$
$\simeq$ 9.5 kpc and HWHM$_{5^{\prime}-10^{\prime}}$ $\simeq$ 19 kpc), the pixel scale
(1.9 kpc pixel$^{-1}$ for the $10^{\prime} - 30^{\prime}$ sample and 5.7 kpc pixel$^{-1}$
for the $5^{\prime} - 10^{\prime}$ sample) is sufficiently small to provide
for several pixels of coverage over the detection.  We do not resolve extended
emission along the disk minor axis and therefore, we confine ourselves
to parametrizing the major axis profile.  However,  we can conclude
that the 100$\mu$m emission is confined to within 9.5 kpc of the disk
plane for
the $10^{\prime} - 30^{\prime}$ sample and within 19 kpc for the
$5^{\prime} - 10^{\prime}$ sample (independent of inclination because
these are upper limits).

\begin{figure}
\epsscale{1.0}
\plotfiddle{fig9.ps}{4in}{-90}{70}{70}{-270}{375}
\caption{The simultaneous best fit to the 100$\mu$m surface brightness
profiles of the $10^{\prime} - 30^{\prime}$ sample $({\it left~panel})$ and the $5^{\prime} -
10^{\prime}$ sample $({\it right~panel})$, before renormalizing the errors.  The
surface brightness profiles are modelled by an exponential convolved
with a Gaussian (see text for details).  The $1\sigma$ error bars plotted are
derived from the rms scatter of the mean of the various Monte Carlo
realizations of the control samples.  \label{f9}}
\end{figure}

Along the direction of maximum emission ($0^{\circ} \leq
|\theta| \leq 22.5^{\circ}$), we fit an exponential radial profile to
the surface brightness, a model for the underlying light distribution, convolved with a
Gaussian, a model for the PSF.  Because we do not know the
effective PSF or the exponential scale length of the 100$\mu$m
emission, both the HWHM of
the Gaussian and the exponential scale length, r$_{d}$ are free
parameters.  We
simultaneously fit the data from both samples to the convolved
function by minimizing $\chi^{2}$ (and imposing the conditions that HWHM$_{5^{\prime}-10^{\prime}}$
= 2.0 $\times$ HWHM$_{10^{\prime}-30^{\prime}}$ and that the exponential scalelengths be
the same).  Figure~\ref{f9} demonstrates our best fit,
which is obtained for HWHM$_{10^{\prime}-30^{\prime}}$ = 0.595R$_{25}$ = 11.0~kpc
and $r_{d}$ = 0.13R$_{25}$ = 2.4~kpc, with a reduced $\chi^{2}$ = 2.84.  For
the majority of the 100$\mu$m surface brightness profile, the best fit is generally within
the 1$\sigma$
error bars, which are derived from the rms scatter of the mean
of the various Monte Carlo realizations of the control samples.  More
significant deviations occur in the outer regions of the profile, when
the flux values approach sky levels ($\sim$
1R$_{25}$ for the $10^{\prime} - 30^{\prime}$ sample and $\sim$ 2R$_{25}$ for
the $5^{\prime} - 10^{\prime}$ sample).  Although the errors are
large, we may be seeing evidence for a second, more extended component
at large radius (r$\mathrel{\spose{\lower 3pt\hbox{$\mathchar"218$}$25~kpc).

The task of determining the uncertainties of the parameters is more
difficult than that of identifying the best parameters.  Although some parameters yield good fits that cannot be rejected at a
confidence level $>$90$\%$, neither model has a reduced $\chi^{2} \sim 1$.
Either the model is not entirely representative and there is a
nonexponential tail to the dust emission, or the uncertainties are
underestimates.  We conservatively suggest that $\chi^{2}$ is inflated.  As a result
of details of the polar rebinning procedure, pixels at small radii are
not independent (i.e. for small $r$, one $(x,y)$ pixel
contributes to different $(r,\theta)$ pixels after
rebinning).  Therefore, the calculated rms scatter for pixels at small
$r$ does not fully reflect the uncertainties.  To compensate for this
effect, we now renormalize
the errors in the following manner.  Because the underestimation of uncertainties
is more severe at small radii than at large, we renormalize the
errors using a factor $\propto$ A/r and define A to result in
$\chi^{2} = 1.0$ while fixing the model Gaussian to have 0.585R$_{25} \leq$
HWHM$_{10^{\prime}-30^{\prime}} \leq$ 0.595R$_{25}$, drawn from the
best fit (the IPAC estimated PSF
has HWHM$_{10^{\prime}-30^{\prime}} \sim$ 0.50R$_{25}$).  Using the
renormalized errors and fixing the range of the HWHM, we again
simultaneously fit the models to the data from both samples and find
the following parameter range acceptable within the 90$\%$
confidence level:  0.09R$_{25} \leq$ r$_{d} \leq$ 0.18R$_{25}$ or 1.7~kpc
$\leq$ r$_{d} \leq$ 3.3~kpc.

\begin{deluxetable}{lcc}
\tablewidth{0pt}
\tablecaption{Best Fit\tablenotemark{a}~~Parameters for 100$\mu$m
Surface Brightness Profile Fitting \label{t3}}
\tablehead{
Sample & \colhead{HWHM$_{10^{\prime}-30^{\prime}}$} & \colhead{r$_{d}$}
}
\startdata
10$^{\prime}$ - 30$^{\prime}$ & 0.520R$_{25}$ - 0.650R$_{25}$ &
0.05R$_{25}$ - 0.20R$_{25}$\nl
& 9.6~kpc - 12.0~kpc & 0.9~kpc - 3.7~kpc\nl
\nl
5$^{\prime}$ - 10$^{\prime}$ & 0.565R$_{25}$ - 0.610R$_{25}$ &
0.05R$_{25}$ - 0.20R$_{25}$\nl
& 10.5~kpc - 11.3~kpc & 0.9~kpc - 3.7~kpc\nl
\nl
Simultaneous fits to & 0.585R$_{25}$ - 0.595R$_{25}$ & 0.09R$_{25}$ -
0.18R$_{25}$\nl
both samples & 10.8~kpc - 11.0~kpc & 1.7~kpc - 3.3~kpc\nl
\enddata
\tablenotetext{a}{Within 90\% confidence level}
\end{deluxetable}

One important result that may be casually overlooked is the significance
of simultaneously fitting the data from both samples to the same
exponential.  One might naively expect that dust should be detected in
either sample out to the same radius, particularly since, as pointed
out previously, the galaxies
in these two samples do appear to be the same type of galaxies
($\langle$R$_{25}\rangle \sim 18.5$~kpc for both samples).  However, due to the differences
in sample size, the mean distance of galaxies in the two samples, and
the effect of the PSF on samples of different angular size,
the sensitivities are not the same.  Separate fits to the two samples
yield the $90\%$ confidence parameter ranges given in Table~\ref{t3}.  The range of
acceptable parameter space allowed by fitting the two samples separately
is consistent with that allowed by simultaneously fitting both samples
and with each other.

How does our derived 100$\mu$m emission scalelength compare to that
of the stellar component in a typical disk galaxy?  The most recent
and complete study of stellar disks is that of de Jong (1996a, 1996c), who uses
near-infrared and optical broadband surface photometry of 86 face-on,
disk dominated galaxies to investigate the distribution of disk and
bulge parameters.  Because K-band light is less affected by dust
obscuration than B-band light, we choose to compare our result to the
distribution of K scalelengths which range from $\sim$~1~-~10~kpc,
with a median of $r^{K}_{d}=$3.8~kpc~,
and a rms dispersion of 2.4~kpc (for H$_{0} = 75$~km/s/Mpc).  However, the distribution of
scalelengths is a positive definite quantity with a significant
high-end tail that is not described
by a Gaussian.  Therefore, the median is biased to a larger value
than the peak of the distribution, which is quite broad and is in the range
$\sim$ 2~-~4~kpc ($40\%$ of the galaxies have scalelengths in this
range).  This range overlaps the $2.5\pm0.8$~kpc range of 100$\mu$m scale
lengths that we measure.  Because de
Jong finds no correlation of scalelength with galaxy type, any differences in the distribution of galaxy type between the optical
study and our samples is unimportant.  We conclude that the
derived 100$\mu$m scalelength is most likely not much larger than that of the
underlying old stellar component and is consistent with being equivalent
to or up to a factor of two smaller than that of the stellar distribution.

\subsection{A Simple Model for the Dust Distribution}

The characteristic scale length of the 100$\mu$m emission
derived in the previous section can be used, in conjunction with
simple modelling, to place a limit on the global dust
mass distribution.  Because we have data in a single passband with
poor spatial resolution, we follow the procedure
of Bothun $\&$ Rogers (1992), who use a one-component model (a single
blackbody with characteristic temperature) to
describe the far-IR emission from dust, based on 60$\mu$m and 100$\mu$m
IRAS images.  The one-component assumption
is questionable because of different
temperature dust components needed to
fit observed far-IR spectral energy distributions.  Some find that
multi-component models are needed to explain their far-IR observations
(e.g. Helou 1986; Rowan-Robinson \& Crawford 1989; Andreani \& Franceschini 1996), while
others concur with Bothun \& Rogers (1992) and find that their far-IR spectra can be well fit by a single component
model (e.g.  Sodroski {\it et al.\ } 1994; Clements, Andreani and Chase 1993;
Odenwald, Newmark and Smoot 1996).  Using DIRBE all-sky data, Sodroski {\it et al.\ } (1994) showed that a
ubiquitous far-IR component can be detected as a single component at $60 \mu m < \lambda <
240 \mu m$ with $17 K < T_{d} < 22 K$ that is closely
associated with the far-IR cirrus discovered by IRAS at 100 $\mu$m.
Studies of IR selected galaxies find that the galaxies' continua are
consistent with a single component model with
25~$\mathrel{\spose{\lower 3pt\hbox{$\mathchar"218$}~$T$_{d}~\mathrel{\spose{\lower 3pt\hbox{$\mathchar"218$}$~35, and a peak emission near
100$\mu$m (Clements, Andreani and Chase 1993; Odenwald, Newmark and Smoot
1996).  While dust certainly exists at a variety of temperatures, we
use a simple one component model because of the limited temperature
information provided by our single band data, and the evidence that
the far-IR continua of the 100$\mu$m emitting dust is well fit by a
single temperature blackbody in the range 20~K $\mathrel{\spose{\lower 3pt\hbox{$\mathchar"218$}$ T$_{d} \mathrel{\spose{\lower 3pt\hbox{$\mathchar"218$}$
35~K.  Subsequent observations at mm wavelengths will be necessary to test this
assumption.

Bothun $\&$ Rogers (1992) model the 100$\mu$m emission using an
isothermal dust slab at a dust temperature, T$_{d}$, that is optically thin to
far IR emission.  They assume that within each region of the disk sampled by
a pixel, radiative equilibrium exists between the interstellar
radiation field (ISRF) and the dust grains, and also that the ISRF,
represented by mean intensity, J$_{\nu}$, is uniform over the region.
They derive the following relationship between ${\it f}_{\nu_{0}}$, the observed flux
density in an IRAS passband with effective frequency $\nu_{0}$, and the
integrated mean intensity J:
\begin{equation}
{\it f}_{\nu_{0}}~\propto~{\cal F}_{\nu_{0}}(T_{d})\tau_{J} J,
\end{equation}
\noindent where $\tau_{J}$ is the mean-intensity-weighted optical
depth of the dust and
${\cal F}_{\nu_{0}}$ is the fraction of the total emission contained
within the IRAS band.  For a power law dust emissivity law that is proportional to
$\nu^{p}$, ${\cal F}_{\nu_{0}}$ can be expressed as
\begin{eqnarray}
{\cal F}_{\nu_{0}}~=~\int_{0}^{\infty} {{x^{3+p}}\over{e^{x}-1}}R_{x}dx/[\Gamma(4+p)\zeta(4+p)],
\end{eqnarray}
\noindent where $x=h\nu/kT_{d}$, R$_{x}$ is the system response
for the band that is tabulated in the IRAS Explanatory Supplement, and
$\Gamma$ and $\zeta$ are the Gamma and Riemann Zeta functions.

Because $\tau$ is proportional to mass in the optically thin regime, we can use the above
equations to trace dust mass as a function of radius if we know the dust
temperature profile, the 100$\mu$m light profile, and the integrated
mean intensity profile of the ISRF.  The radial profile of the dust mass
distribution can be derived without needing to derive the various coefficients which are difficult to
determine empirically.  We assume that
\begin{equation}
J~\propto~exp(-r/r_{s}),
\end{equation}
\noindent where $r$ is the radius and $r_{s}$ is the scale length of
the stellar component.  In the previous section, we determined that
the 100$\mu$m emission is also described by an exponential and thus
\begin{equation}
{\it f}_{\nu_{0}}~\propto~exp(-r/r_{d}),
\end{equation}
\noindent where $r_{d}$ is the 100$\mu$m emission scale
length.
The only term in these equations that depends on the dust temperature
is ${\cal F}_{\nu_{0}}$.  Bothun $\&$ Rogers (1992) using 60$\mu$m and 100$\mu$m images for 28 nearby galaxies, found
that the dust temperature declines radially, due
to the exponentially declining ISRF.  These authors modeled the
temperature profile with an
exponential
\begin{equation}
T_{d}~\propto~exp(-r/r_{d}),
\end{equation}
\noindent which, for a limited range of scalelengths, can be approximated by a drop of 3 K for every optical
scale length (Bothun \& Rogers 1992).  This temperature profile is consistent with their
data out to a radius of $\sim$ 3 optical scalelengths, where the
temperatures converge to a near constant value of $\sim$ 28 K (Bothun
$\&$ Rogers).
Therefore, we use the exponential temperature gradient, normalized to produce $T_{d}$ = 34.9 K at one optical
scale length and converging to a constant temperature of 28 K for $r >
3r_{s}$.

We can now solve for the dust distribution once we adopt values for the
100$\mu$m emission scale length, $r_{d}$, and the scalelength of the
stellar component, $r_{s}$.  For $r_{d}$, we choose the mean of the
two best fit values, $r_{d}$ = 2.5~kpc.  As discussed previously, the
100$\mu$m scalelength could be equal or up to a factor of $\sim$2 smaller
than the stellar scalelength.  Thus, we investigate the regime $0.5 \leq
r_{d}/r_{s} \leq 1$.  When $r_{d}/r_{s}~=~1$, the model
predicts a slight fall in the dust mass distribution in the inner
regions of the galaxy (due to the radial temperature gradient)
and then the dust mass distribution flattens out when the temperature
converges to a constant.  In the absence of a temperature gradient, the distribution is flat at
all radii.  This result occurs because Eq. 1 simplifies to
$\tau \propto 1/{\cal F}_{\nu_{0}}(T_{d})$, for equal stellar and dust
emission scalelengths.  If
the temperature is constant with radius, then ${\cal F}_{\nu_{0}}$ is
constant, and $\tau$ is independent of radius.  For $0.5 \leq
r_{d}/r_{s} < 1$, an exponentially declining dust mass with radius is predicted, with
the dust being less centrally concentrated than the stars.  As
$r_{d}/r_{s}$ decreases, the dust mass scalelength decreases until it equals the stellar emission scalelength for
$r_{d}/r_{s} = 0.5$.

A flat or slowly declining exponential radial dust distribution is consistent with
the findings from optical studies.  de Jong (1996b) studied the optical and infrared
color profiles of 86 face-on disk-dominated galaxies using models of
well mixed stars and dust that include both scattering and
absorption.  He found that high central
optical depths and long dust scalelengths best reproduced the
observed color gradients.  However, he cautions that a realistic dust
distribution alone cannot
adequately account for the observed gradients, and that
stellar population characteristics, namely age and metallicity gradients, need
to be incorporated.  Peletier {\it et al.\ } (1995) also studied
spiral galaxies in the optical and infrared using models of smoothly
distributed dust and stars that only included absorption, but also
concluded that $r_{d}/r_{s} > 1$.  However, when they included scattering and
clumpiness in the dust models, $r_{d}/r_{s} \geq 1$ yielded acceptable
solutions.

\subsection{Implications of the Dust Mass Distribution}

How does the dust distribution compare to other galaxy components?
Neutral hydrogen has a radially flat distribution (Shaya $\&$ Federman 1987), while molecular gas appears to
decline exponentially (e.g.  Young $\&$ Scoville
1991).  Because our data cannot distinguish between a flat or
exponentially declining distribution of dust, we will discuss both
cases.  Some authors find a good correlation between
FIR luminosities and the distribution of molecular gas (e.g. Devereux $\&$
Young 1990a, 1990b, 1992, $\&$ 1993, Tinney et
al. 1990, Sanders {\it et al.\ } 1991, Downes {\it et al.\ } 1993, Sage 1993).  Devereux $\&$ Young
(1990a, 1990b, 1992, $\&$ 1993) studied the origin of the FIR
luminosity in IR luminous spiral galaxies and concluded that FIR luminosity is an
excellent indicator of star formation, being well correlated with
H$\alpha$ luminosity and the surface density of H$_{2}$ (as
inferred from CO observations) and poorly correlated with the surface
density of HI.  These authors claim that their observed FIR
luminosities are due to the reradiation by warm dust of
UV flux from young OB stars in HII regions, and therefore, the dust
exponentially declines with radius as do the stellar and molecular
components.

Others provide
evidence for a second cooler, more diffuse cirrus-type component,
that is associated with the HI rather than star
forming regions and excited by the ISRF from old disk stars.  Using a model that includes both components, Lonsdale-Persson $\&$
Helou (1987) have calculated that cirrus-type emission can account for
up to between 50\% and 70\% of the total FIR emission from a median spiral
galaxy, and subsequent observations have supported their claim
(Walterbos \& Schwering 1987, Rice {\it et al.\ } 1990, Sauvage \& Thuan 1992,
Xu \& Helou 1996).  Furthermore, Sauvage \& Thuan (1992) observationally determined that
the fractional contribution of cirrus-type emission to the total FIR
of spiral galaxies is a function of type:  $\sim 3\%$ for Sdm,
increasing to $\sim 70\%$ for Sc galaxies, and reaching as high as
$\sim 86\%$ for Sa galaxies.  When normal spiral galaxies (i.e. not ultra luminous
IRAS galaxies nor active galaxies) are studied, the contribution from
the cirrus component becomes important and non-negligible
correlations between cold dust and HI are found, although cold dust is
better correlated with the total gas content (HI + H$_{2}$) than with either
phase separately (e.g.  Knapp, Helou, \& Stark 1987, Andreani, Casoli,
\& Gerin 1995, Xu \& Helou 1996).  Xu \& Helou (1996) studied the
diffuse component of the FIR emission of M31 by removing FIR emission
associated with HII regions and found a close association of the
diffuse cirrus-type component with HI, while a poor correlation was
found with H$_{2}$.  Interestingly, these authors calculate the radial
behavior of the V-band optical depth, $\tau_{V}$, and find that the
overall distribution of $\tau_{V}$ is rather flat out to a radius of
$\sim$ 14~kpc.

Because the galaxies in our samples are
predominantly of type Sc and earlier, we expect the cirrus component,
rather than the dust component associated with HII regions,
to be the main contributor to the FIR emission.  However, a number
of authors have demonstrated that IRAS is not very sensitive to
emission by cold dust and that the emission from large amounts of cold
dust can easily be dominated by emission from a small amount of warm
dust (e.g. Bothun $\&$ Rogers 1992, Sage 1993, Block {\it et al.\ } 1994).
In reality, the 100$\mu$m emitting dust detected in our sample is probably associated, at some level, with both the molecular and atomic gas phases.  While our assumed dust
temperature of $\sim$30K is similar to dust temperatures derived for
samples of nearby spirals (e.g.  Young et al 1986, Walterbos \& Schwering
1987, Jura 1986, Bothun \& Rogers 1992), this is not the
characteristic temperature of either HII regions, which are hotter, nor the HI
interstellar medium, which is typically colder.  Our assumed dust temperature was
derived by Bothun \& Rogers (1992) using a single temperature model,
based on 60$\mu$m and 100$\mu$m data with very coarse resolution where
each pixel samples a wide range of local heating conditions, and
consequently is
probably an average of the temperatures of the two contributing components.  Therefore, although
our data do not allow us to differentiate between a flat and exponentially
declining distribution of dust, the 100$\mu$m emission measured in our
sample almost assuredly originates from both warm dust residing in HII
regions and associated with the exponentially declining molecular gas and also from the cooler,
cirrus component associated with the flatly distributed neutral hydrogen .

Ultimately, we would like to know
the radial extent of the dust layer.  In particular, does it have a
cutoff at some radius?  Unfortunately, our current data do not allow us to answer this
question, but we can use them to place a lower limit on that cutoff radius.  We have detected 100$\mu$m
emission from dust out to a radius of 27 kpc (with $\geq$
2$\sigma$ confidence).  This is a lower
limit to the cutoff radius and large amounts of cold dust
at larger radii could exist.  We can compare this limit to the known
edges of the stellar (e.g.  van der Kruit $\&$ Searle 1981a, 1981b,
1982a, 1982b) and neutral hydrogen (e.g.  Corbelli, Schneider \&
Salpeter 1989, Corbelli \& Salpeter 1993, Bland-Hawthorn, Freeman \&
Quinn 1997) disks.  van der Kruit {\it et al.\ } (1982a) found
that all of the stellar disks in their sample of 8 galaxies have
a sharp edge at 4~-~5 radial
scalelengths, or 14~-~25~kpc with an average value of 17~kpc.  Neutral
hydrogen disks also have a sharp boundary, although at radii beyond the edge of the stellar disk.
For example, galaxies in the Sculptor group have observed HI disks that extend
to $\sim$1.2R$_{25} \sim 23$~kpc (Bland-Hawthorn, Freeman $\&$ Quinn
1997).  Few galaxies have HI disks that extend farther to $\sim$2R$_{25}
\sim$~38~kpc (Bland-Hawthorn, Veilleux \& Carignan 1997,
Bland-Hawthorn, Freeman \& Quinn 1997).  The radial edge of our 100$\mu$m
detection, at a radius of 27~kpc, is beyond 4~-~5 stellar scalelengths
and therefore, beyond the edge of the stellar disk.  We do not
observe far-IR emission beyond the nominal edge of HI disks,
although because our detection is a lower limit, dust may extend
beyond the edge of the HI disk.

If dust is produced by stars, how can dust be found outside the
stellar disk?  One can speculate that it is primordial, i.e.  that it formed early in the process of galaxy
formation and then settled into a disk similarly to the HI, that galactic fountains, plumes of gas and dust ejected by supernovae into
the interstellar medium, pollute the outer galaxy, or that some disk
stars exist at these large radii.  Models of galactic fountains (e.g.  Corbelli
$\&$ Salpeter 1988) show that some of the hot material ejected by violent
supernovae, can rise many kiloparsecs into the halo and then
radiatively cool and fall back toward the outer part of the galactic
plane at distances $\geq$20~kpc.  A similar, but less energetic
mechanism of ejecting dust into the ISM involves radiation pressure
produced by
clusters of young OB stars.  Models of these dusty chimneys by
Ferrara (1995) show that some dust particles can attain rather high
velocities ($\sim$100~km/s) and reach distances of $\sim$3~kpc above
the disk plane.
However, the majority of the dust particles' motion is in a direction
perpendicular, rather than parallel, to the plane of the disk.
The redistribution of dust particles'
in Ferrara's models predicts a flattened dust distribution, which is
consistent with our work (see Fig~\ref{f7}).  Lastly,
although stellar disks are observed to truncate sharply, there is observational evidence for massive star formation in the outer regions
of galactic disks.  Hodge {\it et al.\ } (1988) and Davidge (1993) found blue
stars in two different fields in the outer disk ($\sim$20~kpc) of
M31.  If these
findings are representative of spiral galaxies, then there is at least
some star formation at the very edge of stellar disks which
could contribute dust at large radii.  Therefore, there are several
avenues that need to be more fully explored to determine the mechanism
involved in getting dust to r$\sim$30~kpc.

\section{Summary}

Using 100$\mu$m ISSA images and data from the RC3, we coadd the
flux from 299 galaxies and investigate the radial and azimuthal distribution of
100$\mu$m emission from dust in ensembles of galaxies.  The galaxies are divided into three
samples (where N~$=$ number of galaxies), according to their optical isophotal diameter, D$_{25}$:
(1)~~2.5$^{\prime} \leq$ D$_{25} \leq
5.0^{\prime}$~(N$_{2.5^{\prime}-5^{\prime}} = 184),~(2)~~5.0^{\prime}
\leq$ D$_{25} \leq 10.0^{\prime}~($N$_{5^{\prime}-10^{\prime}} = 91),$ and $(3)~~10.0^{\prime} \leq$ D$_{25} \leq
30.0^{\prime}~($N$_{10^{\prime}-30^{\prime}} = 24)$.  We find the following:

\noindent (1)  that 100$\mu$m emission extends out to
radii of 27~kpc at the 2$\sigma$ or greater confidence level for the
$5^{\prime} - 10^{\prime}$ sample and to
21~kpc for the $10^{\prime} - 30^{\prime}$ sample (no extended
emission is seen beyond the PSF for the $2.5^{\prime} - 5^{\prime}$ sample),

\noindent (2)  that the 100$\mu$m emission from both the $5^{\prime} - 10^{\prime}$ and $10^{\prime}
- 30^{\prime}$ sample is preferentially elongated along the major axis of the
disk, thus confirming the validity of the detections and demonstrating
that 100$\mu$m emitting dust is flattened into the disk,

\noindent (3)  that the 100~$\mu$m surface brightness
profiles from both samples can be well fit with an exponential with a dust
emission scale length of $\sim 2.5 \pm 0.8$~kpc, but there is evidence
for a second, more extended emission component, and

\noindent (4)  that a
model of the 100$\mu$m emission from an isothermal dust slab at
temperature, T$_{d}$, that is optically thin to emission can be used
to model our data (cf. Bothun \& Rogers 1992).  Because our
data do not allow us to calculate dust temperatures, we adopt the dust
temperature gradient derived by Bothun
\& Rogers (1992),
which can be approximated by a drop of 3~K for every optical scale
length, r$_{s}$, and is normalized by T$_{d} = $34.9~K at one optical scale length and
converges to a near constant value of $\sim$28~K for r$~>~3$r$_{s}$.
Using this model, we examine the range of acceptable dust mass
distributions allowed by our data and find that the dust is less
concentrated than the stars, with either a flat or slowly declining
exponential distribution.

We have presented evidence for dust well beyond the stellar
disk, but have been unable to conclude whether dust exists
beyond the extent of the HI distribution.  Such dust, if present, should be quite
cold ($\mathrel{\spose{\lower 3pt\hbox{$\mathchar"218$}$ 10~K) and difficult to detect with IRAS observations,
despite the possible evidence of a second component in our data.  The
future of this field relies on longer wavelength observations.
Preliminary detections of dust at large radii using 200$\mu$m
observations have recently been presented by Alton {\it et al.\ } (1998).  We
await further results from such observations.

\vskip 0.5in
\noindent
Acknowledgments:  DZ acknowledges funding from a NASA LTSA grant
(NAG-5-3501), a NSF
grant (AST-9619596), and the Packard Foundation.  AEN \& DZ gratefully acknowledge financial
support from the Cal Space Foundation.  AEN gratefully acknowledges
financial support from the University of California Graduate Research
Mentorship Fellowship program.  RMC acknowledges the support of the
Jet Propulsion Laboratory, Caltech, which is operated under contract
with NASA.

\clearpage
\centerline{References}
\refbook{Alton, P.B., Davies, J.I., Bianchi, S. \& Irewhella, M. 1998
in ``Galactic Halo: A UC Santa Cruz Workshop'', D. Zaritsky (ed.), (San
Francisco: ASP), p.149}
\aa{Andreani, P., Casoli, F. \& Gerin, M. 1995}{1995}{43}
\mnras{Andreani, P., \& Franceschini, A. 1996}{283}{85}
\apj{Bland-Hawthorn, J., Freeman, K.C. \& Quinn, P.J. 1997}{490}{143}
\refbook{Bland-Hawthorn, J., Veilleux, S., \& Carignan, C. 1997, in prep.}
\aa{Block, D., Witt, A., Grosbol, P., Stockton, A., Moneti,
A. 1994}{288}{383}
\apj{Bothun, G.D., Lonsdale, C.J., \& Rice, W. 1989}{341}{129}
\aj{Bothun, G.D., \& Rogers, C. 1992}{103}{1484}
\mnras{Clements, D.L., Andreani, P. \& Chase, S.T. 1993}{261}{299}
\apj{Corbelli, E. \& Salpeter, E.E. 1988}{326}{551}
\apj{Corbelli, E. \& Salpeter, E.E. 1993}{419}{104}
\aj{Corbelli, E., Schneider, S.E. \& Salpeter, E.E. 1989}{97}{390}
\apj{Davidge, T.J. 1993}{409}{190}
\apjlett{Devereux, N.A. \& Young, J.S. 1990a}{350}{L25}
\apj{Devereux, N.A. \& Young, J.S. 1990b}{359}{42}
\apj{Devereux, N.A. \& Young, J.S. 1992}{103}{1536}
\apj{Devereux, N.A. \& Young, J.S. 1993}{106}{949}
\apjlett{Downes, D., Solomon, P., Radford, S. 1993}{414}{L13}
\mnras{Fall, S.M. \& Efstathiou, G. 1980}{193}{189}
\refbook{Ferrara, A. 1995 in ``The Physics of Galactic Halos'', 156
WE-Heraeus-Seminar, H. Lesch {\it et al.\ } (eds.), (Verlag:Berlin)}
\apj{Fich, M., Blitz, L., Stark, A.A. 1989}{342}{272}
\apjlett{Helou, G. 1986}{311}{L33}
\apj{Hodge, P., Lee, M.G., Mateo, M. 1988}{324}{172}
\aa{de Jong, R.S. 1996a}{313}{45}
\aa{de Jong, R.S. 1996b}{313}{377}
\aa{de Jong, R.S. 1996c}{313}{557}
\apj{Jura, M. 1986}{306}{483}
\apj{Kennicutt, R.C. 1989}{344}{685}
\apj{Knapp, G.R., Helou, G., \& Stark, A.A. 1987}{94}{54}
\aa{van der Kruit, P.C., \& Searle, L. 1981a}{95}{105}
\aa{van der Kruit, P.C., \& Searle, L. 1981b}{95}{116}
\aa{van der Kruit, P.C., \& Searle, L. 1982a}{110}{61}
\aa{van der Kruit, P.C., \& Searle, L. 1982b}{110}{79}
\aa{Lequeux, J., Allen, R.J., Guilloteau, S. 1993}{280L}{L23}
\apjlett{Lin, D.N.C., \& Pringle, J.E. 1987}{320}{L87}
\apj{Lonsdale-Persson, C.J. \& Helou, G. 1987}{314}{513}
\apjlett{Low, F.J., $\it{et~al.}$ 1984}{278}{L19}
\apj{Maloney, P. 1993}{414}{41}
\refbook{Odenwald, S., Newmark, J. \& Smoot, G. 1996 preprint (astro-ph/9610238)}
\aa{Peletier, R.F., Valentijn, E.A., Moorwood, A.F.M., Freudling, W.,
Knapen, J.H., \& Beckman, J.E. 1995}{300}{L1}
\apj{Rice, W. 1993}{105}{67}
\apj{Rice, W., Boulanger, F., Viallefond, F., Soifer, B.T. \&
Freedman, W.L. 1990}{358}{418}
\apjsup{Rice, W., Lonsdale, C.J., Soifer, B.T., Neugebauer, G., Kopan,
E.L. et al 1988}{68}{91}
\mnras{Rowan-Robinson, M., \& Crawford, J. 1989}{238}{523}
\aa{Sage, L.J. 1993}{272}{123}
\apj{Sanders, D.B., Scoville, N.Z., \& Soifer, B.T. 1991}{370}{158}
\apjlett{Sauvage, M. \& Thuan, T.X. 1992}{396}{L69}
\apj{Shaya, E., \& Federman, S. 1987}{319}{76}
\apj{Sodroski, T. $\it{et~al.}$ 1994}{428}{638}
\apj{Tinney, C.G., Scoville, N.Z., Sanders, D.B., \& Soifer, B.T. 1990}{362}{473}
\refbook{de Vaucouleurs, G., de Vaucouleurs, A., Corwin, H.G., Buta, R.J.,
Paturel, G., \& Fouque, P. 1991, Third Reference Catalog of Bright
Galaxies (Springer, Berlin) (RC3)}
\aa{Walterbos, R.A.M. \& Schwering, P.B.W. 1987}{180}{27}
\refbook{Wheelock {\it et al.\ } 1994, IRAS Sky Survey Atlas Explanatory
Supplement, JPL Publication 94-11.}
\aa{Wouterloot, J.G.A., Brand, J., Burton, W.B., Kwee,
K.K. 1990}{230}{21}
\apj{Xu, C. \& Helou, G. 1996}{456}{163}
\apj{Young, J.S., Schloerb, F.P., Kenney, J.P., \& Lord, S.D. 1986}{304}{443}
\refbook{Young, J.S., Scoville, N.Z. 1991, Ann. Rev., 29, 581}
\aj{Zaritsky, D. 1994}{108}{1619}

\end{document}

redpajama_set_name: RedPajamaArXiv


The cottages can be found in various counties around the UK and Ireland, with Cumbria, North Yorkshire, Northumberland, Derbyshire, Fife, Ross-Shire, Perthshire, Inverness-Shire, Isle Of Lewis, Aberdeenshire, Gwynedd, Dyfed, Dorset, East Sussex, Cornwall, Norfolk, Kent, Lanarkshire, Ayrshire, Cambridgeshire, West Yorkshire, Oxfordshire, Isle of Wight and Wexford all getting a mention.
There are a couple of holiday cottages to report on this week. Both the cottages featured are in the Highlands of Scotland, thse cottages are: "Gill Cottage in Crosby Garrett near Kirkby Stephen" and "Sporting Heights in Clows Top near Kidderminster".


* Most popular Siddur in the market!
With: Prayer direction, Zmanim, Holidays, identify day of week and more.
Shows statistical characteristics of the landscape at your location, based on the information of the 'DaarMoetIkZijn' website. Currently only works in The Netherlands.
Triple Video Poker for Android! 3 hands of video poker at once! Eight Video Poker variations: * Jacks or Better * Tens Or Better * Bonus Poker * Double Bonus Poker * Joker Poker * Double Joker Poker * Deuces Wild * Deuces and Joker Wild Statistics for each game.
Psyclone provides a toolkit of HVAC psychrometric calculations, allowing individual processes to be examined and supply air volume, condition or capacity to calculated. Psyclone operates in either metric or imperial units.
Obscure your desktop and let matrix code to invade your phone and now TOUCH THE MATRIX. Work in all devices with all Android versions. P.S. Internet permission used for AdMob spots.
MultiSim manages your dual sim adapter by tracking all sim cards used in the phone. It also displays the provider icon or a custom icon of your current sim card on the notification bar. Dual-sim-adapter users can switch their sim cards with the included Widget. HyperCard 3G, MagicSim 3G (in 007 Mode) and analog adapters are supported.


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text:
Nevis Island Government To Hold Meeting About Crime Wave
Nevis Island Premier – Joseph Parry
In an effort to resolve the existing crime situation on Nevis, the Nevis Island Administration (NIA) and members of the police force will meet with the private sector at the Nevis Credit Union Conference room on Chapel Street in Charlestown at 10 a.m. on Thursday, July 24, 2008.
The panellists for this symposium will be the Premier of Nevis, Hon. Joseph Parry, Junior Minister of Security, the Hon. Dwight Cozier, Cabinet Secretary in the Nevis Island Administration, Mr. Ashley Farrell, Legal Adviser, Hon. Patrice Nisbett and Superintendent of Police in Nevis, Mr. Samuel Seabrooks.
"We look forward to the participation of all parties as we strive to preserve a peaceful Nevis," said Premier Parry.
Mr. Parry went on to say, that he is confident that out of this meeting will come some positive ideas and solutions, so that crime does not increase and become rampant on the island.
Categories Nevis News Tags Crime In Nevis, Economy, Tourism
St. Kitts – Nevis Cabinet Moves Closer On Minimum Wage
Nevis Citizens To Get Reduced Halthcare Rates

redpajama_set_name: RedPajamaCommonCrawl


text:
Angelo Maria Bandini, född den 25 september 1726 i Florens, död den 10 augusti 1803 i Fiesole, var en italiensk bibliograf och filolog.

Bandini, som var bibliotekarie vid det laurentinska biblioteket i Florens, utgav flera viktiga bibliografiska arbeten, bland annat Catalogus codicum manuscriptorum bibliothecæ mediceæ laurentianæ (1764–1793) och De Juntarum typographia (1791), samt upplagor av de grekiska klassikerna.

Källor

Italienska bibliotekarier
Italienska filologer
Bibliografer
Filologer under 1700-talet
Italienska forskare under 1700-talet
Personer från Florens
Födda 1726
Avlidna 1803
Män
Ugglan

redpajama_set_name: RedPajamaWikipedia


If you're looking for a function to align tables, there is an Align menu. Select two or more tables, to activate the menu. Then you can align tables as you like.
If you're looking for a function which will automatically lay out your tables, we do not plan to add this feature. Deciding where to put a table is part of the design process and it shouldn't be automated.
Whilst I agree to a point that table placement is part of the design process, I for one value visual clarity of my model over functional organisation. Lines crossing is just wrong!
Especially when you want to switch from any other tool to vertabelo and you import an existing database, this becomes a critical feature. The subject areas are not allowing to create relationships or copy existinng relationships into them is another problem.


text:
Shri Alkheswar Mahadev Mandir is a sacred temple of Alkheshwar mahadev otherwise known among locals as Alakh Baba.

The temple is located in the village of Bera, in the Mathura District in the Indian state of Uttar Pradesh. It was constructed by Jayas in ancient times.

The Temple Complex

The complex has two big entry gates, one being used more often. There are temples of all the major Gods. The main temple is dedicated to lord Shiva while others are of deities like Ram, Sita, Ganesha, Brahma, Durga, Radha, Krishna, Shani, Hanuman and more. There is a Havan Kund too. The idol of Lord Shiva in the main temple was found in Alkheswar Kund, a nearby water pond. There are different kinds of plants found here. Two motor water pumps serve water to the temple. Drinking water is available to the devotees. On the distant corner of the complex there is a public toilet. A vast playground separates the toilet from the main temple area. A lot of children and teenagers can be seen here playing in the evening.

Festivals

A fair is organized in the month of march every year. The fair being held inside the temple complex is organized by Alkheshwar Mandir Samiti. The temple and pond are centers of religious activities. From early in the morning till late evening devotees can be seen all around the temple. During the Hindu festivals like Holi and Diwali the temple attracts huge crowds. Mahashivratri attracts the most. The music and dance during Mahashivratri leave no one unattached.

Alkheshwar Kund

It is a very big pond adjacent to temple complex. A lot of water life dwells in it. Many kind of fishes, snails, snakes, turtles can be seen here. Fishing has been permitted in the pond by the gram panchayat. There are old wells in middle of the pond. On the other side of the pond there are large pastures. Local shepherds graze their cattle there. Various kinds of migratory birds can be seen here in winters.

References
Konow, Sten. Editor. 1929. Kharoshthī Inscriptions with Exception of those of Asoka. Corpus Inscriptionum Indicarum, Vol. II, Part I. Reprint: Indological Book House, Varanasi, 1969.
Growse, F. S. 1882. Mathura A District Memoir
Drake-Brockman, D. L. 1911. Muttra A Gazetteer.
Harendra Singh

External links

 Details about Mathura

Hindu temples in Mathura district


Last major engine of this kind available, out of production at Polini. A complete kit 70cc aluminum, 47mm diameter, 6 transfers, large exhaust W ... for guaranteed performance. Cylinder kit Franco Morini G304-303 suitable for the Malaguti Fifty 50 Top.


text:
Netflix/YouTube
Netflix cancels Michelle Wolf's talk show via Twitter
One website wrote: 'Too bad, so sad.'
Joseph Knoop
Published Aug 18, 2018 Updated May 21, 2021, 8:30 am CDT
After only four months, Netflix is pulling comedian Michelle Wolf's new talk show, The Break with Michelle Wolf.
As if that weren't bad enough for the show's staff, the staff only found out via Twitter, according to a source who spoke with the Daily Beast.
"None of us can believe how classlessly Netflix has handled this," the source told the Daily Beast.
Netflix also canceled The Joel McHale Show, with various reports citing sources that say neither show secured enough consistent viewership to merit a renewal.
Wolf became a household name with her segment during the White House Correspondent's Dinner in April. Wolf, who has previously worked on Late Night with Seth Myers and The Daily Show, provided a scathing takedown of President Donald Trump and his administration, most notably Press Secretary Sarah Huckabee Sanders.
"She burns facts and then she uses that ash to create a perfect smokey eye," Wolf said. "Like maybe she's born with it, maybe it's lies. It's probably lies."
Wolf started the dinner event with a direct reference to Trump's history of sexual assault allegations.
"Here we are at the White House Correspondents' Dinner," Wolf said. "Like a porn star says when about to have sex with [Donald] Trump: Let's get this over with."
Wolf's jokes prompted a large amount of backlash from legacy media members, including the New York Times' Maggie Haberman. Trump later called for the event to be canceled, criticizing Wolf and previous host Seth Myers. The White House Correspondents Association also apologized for the comedian's comments.
The ensuing controversy skyrocketed Wolf to stardom, providing her Netflix show a level of notoriety perhaps uncommon for an internet comedy talk show.
Conservatives critics are reveling in the demise of Wolf's show. Breitbart News included the Twitter headline "Too bad, so sad." Actor and anti-LGBT propaganda propagator James Woods tweeted "Aborted" with a link to the story.
H/T Daily Beast
*First Published: Aug 18, 2018, 11:17 am CDT
Joseph Knoop is a gaming writer for Daily Dot, a native Chicagoan, and a slave to all things Overwatch. He co-founded the college geek culture outlet ByteBSU, then interned at Game Informer, and now writes for a bunch websites his parents have never heard of.
Chris Evans' nonpartisan website reamed for upcoming series on the Middle East
Elon Musk dragged for his 'space represents hope' tweet
Photos show Ted Cruz flying to Cancun amid Texas winter storm crisis (updated)
After Biden's inauguration, people online are still processing the last 4 years


text:
← Don't look in the basement at home because they're watching
STREAM QUEEN: for the love of short running times…or not in some cases →
Camp Massacre – this fat farm slasher needs to slim down
Posted on August 5, 2016 by Daniel
Camp Massacre comes via one of those "horror circles" of indie filmmakers. Most directors/actors/writers involved have all worked together on various projects—most notably, the films The Hospital and The Hospital 2. Someone in the film can even be seen wearing a The Hospital T-shirt.
Despite the hot babes on the poster art, the premise of Camp Massacre is that obese guys competing on a weight-loss reality show get hacked up by a killer wearing a "Six Pack Abs" cooking apron and a fast food chicken bucket as a mask. In fact, after an opening kill with ex-porn star Bree Olsen in a shower, there are pretty much only two females in the entire movie. This slasher comedy is actually a big beary sausage party! There are plenty of huge tits and swollen nipples, but they're all covered in fur!
How's that for falsely advertising to young straight teen boys? Even the title is more geared toward the poster art than the actual plot of the film. Frankly, the title bites big bear boobs no matter what gender is being killed. Camp Massacre? Really??? The film was originally titled Fat Chance, which is equally crappy since it speaks to the "fat" aspect of the film but not the horror. Despite the PC world we live in these days, this big-bellied bear says fuck it. They should have owned it and just called the film Fat Farm Massacre.
But that's not even the major problem with Camp Massacre. The truth is, considering there are dozens of people involved with this film that have done other horror movies and clearly love the genre, it is inexcusable that this one runs two hours and nine minutes long. Fucking INEXCUSABLE.
Don't get me wrong. There are some funny parts that made me laugh out loud, but in between the chuckles—and kills—there are so many plodding, unnecessary segments that drag the film into the amateur zone, making it a chore to hang in there. And considering the kills are not presented as suspenseful or scary (they just—happen, thankfully without CGI), the film desperately needed to rely on its more humorous, exploitative moments to make it fun, keep the momentum going, and tighten up the lag between death scenes. Easily 40 minutes could have been cut from the film without compromising the plot (for instance, the excessive number of lengthy exercising montages).
Now for the highlights of the film. For starters, there's the animated intro. I always love me some animated horror movie intros, and this one features a punk perfect song called "Make the First Move." All the songs in the film have a good 80s movie soundtrack throwback sound.
There are also some familiar faces, including Dick Warlock (Michael Myers in the original Halloween II), brief cameos by scream king Shawn C. Phillips and Scott Tepperman of Ghost Hunters International, and wrestler Al Snow.
From the moment Snow comes on the scene as a boot camp trainer (in a tight tank to show off his beefy bod), he shines. His part is shamefully small considering he brings some of the strongest humor. Also underutilized in terms of delivering the best comic moments are a gay character and a goth character (who also seems pretty gay).
Since this is a sausage party, there's an abundance of flesh to go around. There are plenty of huge, bare bear bellies on display. For fans of lean meat, there's a ripped, pretty boy trainer dressed in a fantastically tight and skimpy exercise outfit right out of the 80s.
And in a unifying boys & bears moment, the trainer even milks some moobs for the milk chocolate hidden underneath.
Jim O'Rear, co-director of the film who also has a role in the film, gets a sex scene in which he wears only a tie and shows off his booty, but the camera sadly never pans below the pube line.
Finally, one of the biggest bears in the bunch lies big belly up for a campy sex scene.
If only Camp Massacre had brought all its best elements closer together by…um…trimming the fat, it could have been a great party movie—and possibly even a cult classic with the gay bear crowd.
I am the author of the horror anthologies CLOSET MONSTERS: ZOMBIED OUT AND TALES OF GOTHROTICA and HORNY DEVILS, and the horror novels COMBUSTION and NO PLACE FOR LITTLE ONES. I am also the founder of BOYS, BEARS & SCARES, a facebook page for gay male horror fans! Check it out and like it at www.facebook.com/BoysBearsandScares.
View all posts by Daniel →
This entry was posted in Johnny You ARE Queer - Gay Thoughts, Movie Times & Television Schedules - Staying Entertained, Scared Silly - Horror Comedy and tagged Camp Massacre, gay horror, horror comedies, slashers. Bookmark the permalink.
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Q: how to debug a web application in chrome? I want to know how we can debug a application ex: facebook in chrome, how we can stepover each backend actions when we login into facebook. How the flow goes in backend when we login into FB...
can we do this in chrome without setting it any breakpoints ?

A:
can we do this in chrome without setting it any breakpoints ?

As far as I know, it cannot be done. If you want to debug your project, you have to set breakpoint. Besides, you should have the sample and should use the localhost to debug it.
First of all, you should open the prject on VS and then debug it with Chrome.
1), when you debug an asp net project, it usually have naming rules. If you open a new form page in Chrome, you can find the related page on the solution explorer, and set a breakpoint on the top of it.
2) Chrome can only debug Javascript code. If you want to debug it, you should press F12 on Chrome to open the developer mode. You can see that the JS code of the current page is under the Source menu, you can set a breakpoint directly at the beginning of the script.

Then you can click on the UI button or menu to start debugging(both js and backend activity ). Also, when you enter a new  form page, just follow the above two steps to debug it.
In addition, since VS2017, you can just debug js in VS, enable option Enable Javascript debugging for Asp.Net under Tools-->Options-->Debugging-->General.
Then, you can search under the solution explorer, find the current debug form page-->find the related js file, and set a breakpoint on the top of it. After it, you can start to debug the menu of asp net project.
Note: every time you enter a new page, you should search both front end and back end pages to set a breakpoint manually.

redpajama_set_name: RedPajamaStackExchange


A concern for the low and moderate income elderly in need of adequate housing moved LLF members to sponsor, in 1960, creation of Fellowship Square Foundation, Inc. (FSF), a not-for-profit corporation to implement Federal housing legislation designated to relieve this need. FSF currently has five buildings on four campuses as detailed below.
Funding for the first project, the 140-unit Lake Anne Fellowship House, Reston, Virginia, was obtained in 1969 through diligent efforts of LLF members. Construction began in February 1970, and the first tenants moved in on May 2, 1971. The Rev. Dr. John A. Scherzer provided imaginative, capable leadership, and the Lake Anne project has been recognized as an exemplary implementation of the Housing Act by the Department of Housing and Urban Development. A wing of 100 apartments, plus facilities for congregate food service and a meeting room to seat 225 persons, was opened for occupancy on October 15. 1976.
The FSF, jointly with the Virginia Housing Development Authority, began construction of Hunters Woods Fellowship House in Reston in May 1970. This facility has 224 apartments plus a crafts room, classroom for continuing education, food service space, and general meeting room. The first residents moved in on March 5, 1979. By June 30, all apartments were occupied with a long waiting list. The project is a part of the central core of Hunters Woods Village, including shops, public library, and the Community Center.
Lake Ridge Fellowship House, located south of Woodbridge, Virginia, opened on July 10, 1983, with 100 apartments for low-income elderly and physically challenged. By September it was fully occupied, with a waiting list.
The Largo Landing Fellowship House opened with 106 units in June 1984. Located in southern Prince George's County, Maryland, this project was a cooperative effort with the Riverdale Baptist Church. These new apartments were quickly occupied, with a waiting list.
Also in 1984, the FSF tested a new phase of service, managing Lewisville Senior Center for Fairfax County's housing authority. This apartment facility was located on the second floor of a former public school; the first floor had been converted to a senior center. A decision by the county to do its own staffing in 1988 brought this test to an end.
Recognizing the need of many older persons for additional support services beyond those independent living facilities, the FSF started construction of Tall Oaks Fellowship House in Reston in 1987. After various construction delays, the first three floors of the facility were opened and staffed. After completing the structure and finding marketing to achieve full occupancy difficult, the facility was sold in 1991 to an owner who could achieve full use of services.
The FSF created a network of corporations during 1988 to facilitate record keeping necessary for the many different financial arrangements required under the laws governing federal, state, and local housing authorities.
The Rev. Dr. John A. Scherzer resigned in late 1988 from the presidency of the FSF. Dr. C. David Hartmann was elected to succeed Dr. Scherzer. Dr. Hartmann was succeeded in 1993 by Floyd E. Anderson. In 1990 Executive Director Leo C. Berger resigned. The Rev. David I. Heeter was elected as Executive Director in 1990. Dr. Heeter resigned his employment with Fellowship Square Foundation in 2000. He was succeeded in late 2000 by Mr. James Garrett. In 2004 Mr. Floyd E. Anderson was succeeded as president by Dr. C. David Hartmann.
There are between 75 and 90 Corporate Members of FSF that are elected by the LLF membership; 25-30 each year for a term of 3 years. Their duties include electing the Board of Directors of FSF.


Large black faux leather tote / shoulder bag with a laser cut style pattern.
Fully fabric lined inside, 2 internal pockets, one with a zip fastening and the second pocket is a slip pocket.
Measurements : approx. 17.5 inch / 43.5 cm wide ( Max. ) 12.5 inch / 31.5 cm high, approx. 5 inch / 11.5 cm in depth at the base.


international radio broadcaster, Radio Taiwan International has experienced many changes over the course of ROC history and left its own sparkling record of accomplishment.
Radio's power is unrestrained by distance. It provides a comforting beacon for listeners and a voice that inspires. Through its broadcasts in 14 languages, RTI reaches audiences around the globe. It has been broadcasting for nine decades, yet has managed to keep pace with the times. Today it uses digital audio and visuals to inform listeners and is committed to covering environmental issues.
An important mission for RTI is to house a collection of voices from history. The station began broadcasting from the then ROC capital of Nanjing at dusk on August 1st, 1928, during a time of momentous political turbulence, and offered listeners a bold new voice. From then on, RTI covered every major event in the Republic of China's history.
After the ROC government withdrew to Taiwan, RTI assumed overt political responsibilities, becoming the voice of "Free China" from Taiwan. Its daily broadcasts were aimed at the Chinese mainland, where they sought to win hearts and minds.
From the beginning RTI broadcast in multiple languages, winning it listeners the world over. "This is one of our greatest advantages and most precious assets," the current RTI chairperson, Lu Ping, says with pride. RTI is now relying on those linguistic resources to build bridges to Southeast Asia and to broadcast to Taiwan's 500,000 Southeast-Asian immigrants.
"Our resources are extremely limited, but we have been able to leverage our strengths," Lu says. Relying on its language capabilities and its many years of experience, RTI has been able to establish relationships with radio broadcasters in Europe that help enhance Taiwan's visibility internationally. On September 27th, 2018, the International Conference on Achieving Sustainability in the Asia-Pacific was held in Taipei, and RTI made an impression at the international media gathering.
"President Tsai Ing-wen made time to attend the event to express support for RTI," Lu says with modesty.
In 2017 RTI representatives attended an event hosted by the Association for International Broadcasting in the United Kingdom, where they invited the AIB's chief executive to visit Taiwan to set the stage for the international sustainability conference. "This was the first time the AIB bestowed its Asia‡Pacific Sustainability Awards, the first AIB awards ceremony to be held outside of the UK, and the first time that the AIB cohosted an international event with an Asian media organization," Lu says.
These successes were the result of RTI's courage to meet new challenges and its unflagging persistence. "This is a momentous achievement, and I'm so proud of my colleagues," Lu says.
If broadcasters want to remain on the cutting edge, they must adapt. "We need to take the bull by the horns and develop better audiovisuals and use the Internet to reach an international audience," Shao says.
In 2017 RTI was nominated for 11 national and international awards and returned with five prizes. A special report on gay families titled "Rainbows in the Sunlight, Lesbians' Children in Taiwan" won an award for best broadcast news feature at the 2017 AIB Media Excellence Awards. It was an affirmation of the excellence of the program and showcased the importance of human rights protections in Taiwan.
At the 2017 Golden Bell Awards, Taiwan's equivalent of the Emmys, RTI's 21:00 Taiwan won first place in the Social Care Program Award and Social Care Award Host categories. The program's report "Listening to Incarcerated Seniors," an examination of aging, had previously won a Brighter Society Journalism award for radio coverage, in 2014. It presented a compassionate investigation of the complexities of aging in the rarely discussed environment of our overcrowded prisons.
"RTI is like a big happy family, with members spanning the globe," says Lu Ping.
A major survey conducted in 2017 by RTI showed that the audience ranges in age from 1 to 100, with more than 66% between the ages of 30 and 60. The RTI site was visited more than 13.45 million times in 2017, and amassed more than 120 million page views, indicating that RTI's 281 programs introducing Taiwan have found a wide audience around the world.
"Once a relationship is established with a global audience it will last a lifetime," says Lu Ping with feeling.
Radio broadcasts seem to elicit the most heartfelt responses from listeners, who come to know the broadcasters and show great loyalty to the programs. Yet after the introduction of digital audio and video, the response has been even more astonishing. In 2017 alone 2.27 million listeners interacted with RTI's programs.
RTI fan group events regularly show high levels of excitement. Members of one mainland Chinese fan group known as the "Fresh Mushrooms" visited Taiwan last year. The members had never met before, and some of them had been listening to RTI for up to 28 years. The group contacted the host of RTI's Stories Behind the Art, who encouraged them to visit Taiwan; after arriving they visited many of the sites introduced by RTI programs, thus becoming more familiar with the island's many wonders.
The conference held for RTI's 90th anniversary addressed the topic of the UN's 17 Sustainable Development Goals, the target date for which is 2030. In the future, according to Lu Ping, RTI will also focus on other important issues in line with its vision for its own sustainable future. "This is just the beginning," she says.
Environmental awareness must be cultivated, and RTI president Shao Li-chung knows from personal experience that the media has a major role to play. "Networking technology will be vital in achieving these goals," he says. Technological innovation has significantly lowered RTI's own electric bills, not only cutting operating expenses but also setting an example in terms of reduced energy use, thus putting the ideal of sustainability into action.
"When it comes to our programming, high-quality content is king," Lu Ping says. And she believes that quality content is the key to continued success.
"We will continue to make use of the power of the Internet, audiovisuals, and multilingualism," says Shao Li-chung.
With a resolute look Shao proclaims that RTI is marching boldly toward another decade of success by adjusting to new challenges, relying on tried-and-true strategies, upgrading technology and reaching new levels of effectiveness. RTI is confidently pressing toward accomplishments for a new age.