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New Hot Topic – Loot Boxes And Their Effect
Viktor Vangelov | Published 17 Sep 2019, 7:52 a.m.
If you have been reading our news articles lately, or pretty much any news source that covers online gambling, you have surely noticed that few topics have dominated the discourse. At least in the UK, we've been discussing issues regarding the status of certain types of gambling and the possibility to introduce stricter regulations.
Problem gambling has been one of the most discussed topics lately, it was featured in the news heavily lately and it was even presented on the popular BBC Panorama. Gambling operators have faced a lot of pressure, from the general public and especially from regulatory bodies and lawmakers who themselves are responding to public pressure. Two weeks ago, leading operators, i.e. their representatives were called at Westminster to discuss issues, including voluntary donations and other ways to combat problem gambling and to promote responsible gambling.
This time we have a different topic that has just surfaced or resurfaced as the hottest gambling-related topic in the UK press – loot boxes.
Loot boxes were discussed in Commons
Video loot boxes are packages that are sold in-game on many games, including games that are aimed at children. Even though loot boxes aren't gambling, in the strict sense of the word, it has been shown that in-game features such as these exploit psychological traits and characteristics that are typically associated with gambling-related behaviours.
Psychologists and other academics are still reluctant to give a definite judgment on loot boxes and their effect on children, seen there's no conclusive data, but many have voiced their concerns over their effects.
The Commons recently discussed loot boxes and the opinion of the House is that loot boxes should be classified as gambling and children should be protected. The Labour Party is known for having a rather negative attitude towards gambling lately, therefore it is not surprising that Labour Deputy and shadow Department for Digital, Culture, Media and Sport minister Tom Watson argued in favour of classifying loot boxes as gambling.
Watson said that the Gambling Act of 2005 should be replaced entirely, so it is evident that the party position has changed dramatically in the last decade, seen that the law was passed by Blair's Labour government.
Multiple arguments and points have been mentioned and explained at the committee meeting, including the issue of purchasing games that are deemed unsuitable for children. It has been argued that same control measures should be applied to online sales as well. If a game can't be purchased on a physical copy, it should not be possible to purchase it online either.
Loot boxes are gambling, DCMS Committee confirms
The Commission did reach a conclusion and the conclusion was that loot boxes come at a high cost for vulnerable groups and expose children to potential harm. The chair of the Committee, Damian Collins said that the said that buying a loot box is like playing a game of chance and that gambling laws should reflect that. He added that Parliament is challenging the Government on the issue and is expecting an answer on why loot boxes should be exempt from the Gambling Act.
The Commission conducted a survey last year and it showed that almost a third of all surveyed children aged 11-16 have purchased loot boxes with one player confessed to spending £1K annually on FIFA in an attempt to get better players.
House Of CommonsLoot BoxesUK Government
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Gambling can easily turn into an addiction and that's why you should always stay in control of the time and expenditure you invest in online gaming. By law, online operators in the UK inform their users about responsible gambling, it is their responsibility to create a legal, fair and safe environment, where players can relax and enjoy the thrill of an online casino safe in the knowledge that they are being treated responsibly.
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We continue our discussion on Black Panther and dive a little deeper into the under lying narratives that surround Wakanda and the African Diaspora.
Today the crew discuss fatherhood and what it means to be a stand up dad. While observing several statistics and studies, the three use their own experiences for a healthy debate on what a good father should be in the black community.
In Episode 16 we introduce our new host, Sheens! We're happy to have her join the team, and she jumps right in to a segment of "Speak Yo Speech" to debate the topic of Black Men Oppressing Black Women, stemming from our Cat Calling episode. We also Introduce our Interview of Rick, Formerly Known as Italia Blue in the Adult-film Industry.
Previous guest from the Black Panther Analysis episode, Mo, returns to "Speak His Speech" on "Blacks in Higher Education".


Has anyone been out with the fly rod? We are going out to the river tonight and I might take mine along and try throwing some streamers. It's my first year with the rod and after seeing how they fought last weekend with a spinning rod, I'm not sure how I'd actually land them. If they are biting good I will probably give it a shot.
Re: Is anyone fly fishing?
Your best bet is to Pm Hebert David,he luvs to fly fish Smallies on the river.Ross is a pro at it.
ON MY INDIAN RUG,AND A PIPE TO SHARE!!!
Thanks Chez, I've only been out on the river 2 times this year, and very limited time while out. I've only used poppers and dry flies so far with limited results. Streamers and wooly buggers should work well but the water up on the North Branch is still a little cloudy. I usually drift them, let them swing, then strip back, alternate the retrieve from fast to slow and see which turns them on.
If you see the Sulphurs and fish are rising have at it, any close imitation will do.
We will shoot thst beaver this year.lol.
had a little time last night so I took the fly rod to the conodoguinet to see if I could catch any, I've yet to get a smallie with it. I tied on an olive and white clouser and had a hit. Unfortunately it broke me off right away. The fish and my fly went off in different directions. After that I tied on a blue version with a lot of flash and had no luck. This is the second fish I've had on that broke off. I don't know what the leader weight is but I may just take that off and tie on some 6 or 8 pound line in its place. my setup is a 5wt.
Its exciting to get a bite but then super disappointing to lose the fish.
You'll be fine with just straight 8lb mono. I have used just straight 8lb or sometimes 10lb mono for years, smallmouth aren't line shy. Walleye and catfish will also hit a clouser in the river. I'm trying out making a twisted leader to an 8lb tippet this season and it turns over a heavier clouser pretty nice.
I go 8-12lb test on my fly line leaders, like Beernut says they are not leader shy. My friend and fly fishing guru Joe Ackourey told me once "The smallies will hit it on a rope" so use the heaviest tippet line you can get through the eye of the hook.
Beernut, are you talking about furled leaders? I've tried them with limited success, I would think for a nicely balance wet fly / streamer set up they would be great, too much wind resistance for my dry flies, I may rig it up and try again if I get on the river anytime soon.
I did one evening this week, the "Hex" flies were out but not in big numbers, I did get one on a top water popper, the Sulphurs were out in good numbers before and after dark but fish just weren't rising for them like they normally do. I did about 15 smallies total and quite a few decent sized ones, all but one on sub-surface.
Chez, I don't think my schedule will allow me any weekends off til who knows when, you will have a good time floating again.
Maybe we can do an early fall trip.
^Oh no!....no time to fish....say it aint so!!
LOL...Get out during the week, it's less crowded anyway.
The lightest tippet I use for river smallies is 3X which is close to 12lb test in strength. No need to go any lighter for fly fishing.
I tie-up and use my own furled leaders, but a store bought tapered leader with a 2' tippet tied on the end works fine. And no leader at all with sinking lines, just 3-4' of straight mono or fluoro.
Haven't been out on the Susky yet this season, but soon. The levels should be coming down and the River should be clearing up this week with the lack of rain.
I grew up fishing the north branch and get up there occasionally, but most times the main river below Harrisburg since it's now closer to home.
I hope to get out sometime next week.
I wanted to thank everyone for the tips, it is working. My casting is getting better and I've managed to catch some fish. All on top water, primarily on a green foam bug thing. I was out last night and on Monday and noticed that about 30 minutes before dark all these flies come out on the water and the fish go nuts. Last night I had a bigger white foam bug which they didn't like as much as the smaller green one. I did hook a decent fish but lost it. Do you guys have any tips for what works best on top water? Also I'm not entirely sure what I'm doing wrong that I lose the fish. I think I'm having trouble keeping tension on the line... Well I know my hook sets are not very good, maybe it is that.
Do you all fish clousers on a 5 weight or is that too light to properly cast? I ask because I feel pretty good with the light lure but the clouser seems like it over loads the rod. Maybe this also just needs practice.
It has been a lot of fun though, top water is just the best.
I was at willow mill, I have not tried the river yet.
Most likely the Clouser is a little too big and/or heavy to cast well on a 5wt. I use a 7wt for smallies on the big rivers. It can handle just about any SMB fly. Your 5 wt should work fine if you keep the flies you cast on the smaller / lighter side.
It sounds like you're doing well with your long stick. It's been a tough year to even get out on the Susky and most of the big rivers in PA with all the rain.
Hopefully the monsoon season ends while the temps are decent.
afishinado… Thanks. I managed to catch a bunch of fish in the last 30-45 minutes of light yesterday. I'm new to fly fishing and I have to say what a blast it is. Still lots to learn, had my leader break where it meets the fly line, it was probably my poor attempt at a nail knot.
Also caught a pretty good size smallie and a big fall fish, just so much fun.


text:
Discover and read the best of Twitter Threads about #thepacificearthquake
Yvonne W
@yvonnewabai
So all the people quoting prophesies in relation to #thepacificearthquake just don't know that Peru is part of the Ring of Fire? Earthquakes are common in Peru. And for y'all to be rejoicing as people die because of some "prophecy"...disgusting. #PeruQuakeProphecyFulfilled #Peru
"The South American Plate is moving over the Nazca Plate at a rate of 77mm/year. Earthquakes occur as thrust faulting on the interface between the two plates. The same process has caused rise of the Andes, creation of the Peru–Chile Trench, and volcanism in Peruvian highlands."
Peru has even had an earthquake of magnitude 9 (1868 Arica earthquake). The most recent earthquake above magnitude 8 in Peru was in 2001 (8.4). In 2007, they had a magnitude 8 earthquake. Peru has had so many earthquakes through the years. It's not prophecy, it's science. #Peru
#Peru #thepacificearthquake #PeruQuakeProphecyFulfilled

redpajama_set_name: RedPajamaCommonCrawl


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text:
Q: Android > Google Maps > Overlay: Tap different things to make different things happen I am trying to make an app where when the user taps on a blank part of the map, a new flag appears, and then when they tap the flag, a dialog box appears.
I wrote the first onTap method on my own, and copied the second from the Google Maps tutorial to get myself started.  The problem is, the first one always fires and the second one never does.  If I delete the first method, the second one works as it's supposed to (tapping a flag makes its corresponding dialog appear).  These are both methods in an ItemizedOverlay class, mContext is the context generated by the constructor, and locations is an ArrayList of OverlayItems.
My question is, how can I reconcile the two?
    public boolean onTap(GeoPoint p, MapView mapView){
        locations.add(new OverlayItem(p, "Point 3", "Point 3"));
        populate();
        return false;
    }

    @Override
    protected boolean onTap(int index) {
      OverlayItem item = locations.get(index);
      AlertDialog.Builder dialog = new AlertDialog.Builder(mContext);
      dialog.setTitle(item.getTitle());
      dialog.setMessage(item.getSnippet());
      dialog.show();
      return true;
    }

A: The problem is that by implementing/overriding onTap(GeoPoint p, MapView mapView) you are preventing ItemizedOverlay's own implementation of that method from running which itself would normally call onTap(int index).
You want something more like...
public boolean onTap(GeoPoint p, MapView mapView){
    if (super.onTap(p, mapView))
        return true;

    locations.add(new OverlayItem(p, "Point 3", "Point 3"));
    populate();
    return false;
}

@Override
protected boolean onTap(int index) {
  OverlayItem item = locations.get(index);
  AlertDialog.Builder dialog = new AlertDialog.Builder(mContext);
  dialog.setTitle(item.getTitle());
  dialog.setMessage(item.getSnippet());
  dialog.show();
  return true;
}

Hope that helps.

redpajama_set_name: RedPajamaStackExchange


text:
\section{Introduction}
\label{intro}

The distribution of stellar masses at star-cluster birth is a complex process not yet fully
understood. Recent observations of the stellar content of star-forming regions in molecular
clouds, rich star clusters and the Galactic field suggest that the initial mass function (IMF)
has similar properties in these very different environments (Kroupa \cite{Kroupa2002}). This
seems to indicate that the initial distribution of stellar masses should depend only on the
process of molecular cloud fragmentation, and that the fragmentation would have to produce
similar IMFs despite very different initial conditions, a physical process which still lacks
a better description (Kroupa \cite{Kroupa2002}). In this sense, detailed analysis of the spatial
structure and stellar-mass distribution in young star clusters may shed light on this issue.
A suitable target for this kind of study is the young open cluster NGC\,6611, which is responsible
for the ionization of the \ion{H}{ii} region Sh2-49 (Sharpless \cite{Sh59}), aka Gum\,83
(Gum \cite{Gum55}) or RCW\,165 (Rodgers, Campbell, \& Whiteoak \cite{RCW60}) as seen in the
optical, or W\,37 (Westerhout \cite{West58}) in the radio.

The open cluster NGC\,6611 (M\,16, Mel-198, Cr\,375, OCl\,54 - Alter, Ruprecht, \& Vanisek
\cite{Alter1970}) consists of a system of early-type stars embedded in emission nebulosity
(The Eagle Nebula) with spatially variable dust attenuation in the optical range. Structurally
the region shows some nebulosity features, the so-called elephant trunks (the ``Pillars of
Creation'', Hester, Scowen, Sankrit, et al. \cite{Hester96}), at the tips of which new-born
stars start to be visible.

The cluster is located at $\ell\approx17^\circ$ and $b\approx0.8^\circ$, in the Sagittarius
spiral arm (Georgelin, \& Georgelin \cite{GG70}), a region presenting conspicuous dense dust
clouds. The whole region is an active site where star-formation processes seem to occur
giving birth to low to high-mass stars (Kroupa \cite{Kroupa2004}). Evidence
has been presented in recent years that NGC\,6611 shows an extremely flat MF (e.g. Sagar \&
Joshi \cite{Sagar79}; Sagar et al. \cite{Sagar86}; Hillenbrand et al. \cite{Hillenbrand93};
Massey et al. \cite{Massey95}). The distance of NGC\,6611 is dependent on the extinction law
but several works constrain it to $\mbox{$\rm d_\odot$}=2.3\pm0.3$\,kpc (Th\'e et al. \cite{twfw90}; Hillenbrand
et al. \cite{Hillenbrand93}; Belikov et al \cite{Belikov99}). The cluster stars have been
observed in evolutionary stages which are not reconcilable with a single age system (de Winter
et al. \cite{w97}). Also, isochrone age determinations are ambiguous for such young clusters
because of the lack of constraints in the CMD morphology. However, several studies show that
the cluster is certainly younger than 10\,Myr with the youngest members still being formed (e.g.
Hillenbrand et al. \cite{Hillenbrand93}; de Winter \cite{w97}; Belikov et al \cite{Belikov00}).
NGC\,6611 presents a significant number of PMS stars. de Winter et al. (\cite{w97}) revised the
subject of PMS membership and related issues by studying PMS candidates individually via photometry
and spectroscopy. They find that the sample objects are not coeval, with an age spread of
$\approx6$\,Myr being necessary to explain the cluster stellar content.

Our main goals with the present work are {\em (i)} carry out a detailed analysis of the spatial structure
of NGC\,6611, {\em (ii)} analyze the spatial variation of the cluster MFs, {\em (iii)} derive properties
of the MS and PMS stars, and {\em (iv)} infer on the dynamical state of this very young open cluster. For
the sake of spatial and photometric uniformity, we employ \mbox{$\rm J$}, \mbox{$\rm H$}\ and \mbox{$\rm K_S$}\
2MASS\footnote {The Two Micron All Sky Survey, All Sky data release (Skrutskie et al. \cite{2mass1997}),
available at {\em http://www.ipac.caltech.edu/2mass/releases/allsky/}} photometry. The 2MASS Point
Source Catalogue (PSC) is uniform reaching relatively faint magnitudes covering nearly all the sky,
allowing a proper background definition even for clusters with large angular sizes (e.g.
Bonatto, Bica, \& Santos Jr. \cite{BBS2004}; Bonatto, Bica, \& Pavani \cite{BBP2004}).

This paper is organized as follows. In Sect.~\ref{m16} we condense previous results on NGC\,6611.
In Sect.~\ref{2mass} we present the 2MASS data, correct the photometry for differential reddening,
subtract the field-star contamination and analyze the CMDs and colour-colour diagrams. In Sect.~\ref{struc}
we discuss the cluster structure. In Sect.~\ref{MF} we derive LFs and MFs and discuss stellar content
properties. In Sect.~\ref{comp} we compare NGC\,6611 with nearby, older open clusters and discuss dynamical
states. Finally, concluding remarks are given in Sect.~\ref{Conclu}.

\section{The young open cluster NGC\,6611}
\label{m16}

The equatorial young open cluster NGC\,6611 is included in the Ser\,OB\,1 association and the W\,37
molecular cloud. It is part of a larger sequence of star-forming events which have just begun in
the region and are still embedded in the molecular cloud (Hillenbrand et al. \cite{Hillenbrand93}).
The cluster contains 8 O\,V-stars (Bosch, Morrell, \& Niemel\"a \cite{Bosch99}).

The first comprehensive photometric study on this object was carried out by Walker (\cite{Walker61})
who obtained UBV photoelectric and photographic observations of NGC\,6611 limited at V=16.7.
He found that in the southern part of the region the colour excess is relatively small,
$\mbox{$\rm E(B-V)$}=0.6$, while to the north the reddening increases irregularly reaching $\mbox{$\rm E(B-V)$}=1.73$. Stars
above the MS were considered possible members in the gravitational contraction phase.
He derived an age of $\rm 1.8\,Myr$ based on the analysis of 532 probable member stars.

Sagar \& Joshi (\cite{Sagar79}) derived a distance to the Sun $\rm\mbox{$\rm d_\odot$}=3.2\pm0.3\,kpc$,
an age in the range 3.0 - 5.5\,Myr, and observed an extremely flat luminosity function in
this open cluster.

Based on photoelectric UBV photometry, Sagar et al. (\cite{Sagar86}) derive a flat MF
with a slope $\chi\approx-0.2$ for stars in the mass range $\rm9\leq m(\mbox{$\rm M_\odot$})\leq70$.

By means of photometric observations over the range from 0.3 to 3.7\,$\mu$m Chini \& Wargau
(\cite{cw90}) provide evidence of an abnormal extinction law only at wavelengths shorter than
0.55\,$\mu$m. They conclude that all PMS stars previously identified by Walker (\cite{Walker61})
present reddening due to normal dust, therefore suggesting that they are foreground objects.

Hillenbrand et al. (\cite{Hillenbrand93}) combined CCD UBV observations with near-infrared JHK
ones to establish a theoretical HR diagram for the cluster, from which they conclude that NGC\,6611
is actively forming 3 - 8\,\mbox{$\rm M_\odot$}\ stars. Using the optical data they infer from a spatial coverage of
$\approx1\,600\arcmin^2$ an overall MS MF slope of $\rm\chi=0.1 - 0.3$ in the mass range $\rm5\leq
m(\mbox{$\rm M_\odot$})\leq85$. It is worth noting that only 4 stars have masses between 40 and 85\,\mbox{$\rm M_\odot$}, for which
they derive an age of $2\pm1$\,Myr. They also present evidence that one 30\,\mbox{$\rm M_\odot$}\ star has been
formed $\sim6$\,Myr ago. They derive $\mbox{$\rm d_\odot$}=2.0\pm0.1$\,kpc.

\begin{figure*}
\begin{minipage}[b]{0.50\linewidth}
\includegraphics[width=\textwidth]{2793fig1a.ps}
\end{minipage}\hfill
\begin{minipage}[b]{0.50\linewidth}
\includegraphics[width=\textwidth]{2793fig1b.ps}
\end{minipage}\hfill
\caption[]{Left panel: XDSS R image. Right panel: 2MASS J image. The area covered in
both images is $1^\circ\times1^\circ$. The small circle at the center of each image
indicates the core, and the large one indicates the size of NGC\,6611 (limiting
radius).}
\label{fig1}
\end{figure*}

By constructing new HR diagrams from the data published by Hillenbrand et al. (\cite{Hillenbrand93})
and applying a different mass calibration,  Massey et al. (\cite{Massey95}) derived an age in the
range 1-5\,Myr, $\chi=-0.3\pm0.2$, and a stellar density of $\rm\rho=5.4\times10^4\,kpc^{-2}$ for
stars above 10\,M$_{\odot}$.

Belikov et al. (\cite{Belikov99}) analyzed the spatial and proper motion distribution of cluster
stars, assuming a normal distribution for the spatial velocities. They derived a distance to the
Sun $\rm\mbox{$\rm d_\odot$}=2.14\pm0.10\,kpc$ and obtained spatial dispersions of $\rm\sigma_{XY}^{core}=1.20\arcmin$
and $\rm\sigma_{XY}^{corona}=4.77\arcmin$, respectively for the core and corona subsystems in
NGC\,6611. They used the same data to measure the differential reddening throughout the cluster
area.

Belikov et al. (\cite{Belikov00}) studied NGC\,6611 based on a compilation of photographic,
photoelectric and CCD optical (UBV) observations covering a circular area of 45.6\arcmin\ in
diameter centered on NGC\,6611. They present radial profiles of the star density distribution in
different azimuthal sectors. Small differences found between the density of the north-west and
south-east sectors were attributed to irregularities of the absorption due to interstellar dust
rather than to stellar density fluctuations. The south-east sector of the cluster is less affected
by dust than the north-west one. The total radial density distribution allowed them to conclude that
virtually no cluster members are present beyond the edge of the cluster corona, at
$\rm 3\sigma_{XY}^{corona}=14.3\arcmin$. They derive an age of 6\,Myr for NGC\,6611. Based on the
number frequency of member stars in the range $\rm 2.1\leq m(\mbox{$\rm M_\odot$})\leq85$ they infer a flat MF slope,
$\chi=0.2$.

Tadross et al. (\cite{Tad2002}) presented an analysis of UBV CCD observations intending to derive
morphological parameters for a large sample of open clusters. For NGC\,6611 they obtained a
colour excess $\mbox{$\rm E(B-V)$}=0.68$, $\mbox{$\rm d_\odot$}\approx1.6$\,kpc, age $\approx3.2$\,Myr, linear diameter
$\rm D=3.6$\,pc, Galactocentric distance $\mbox{$\rm d_{GC}$}=6.94$\,kpc, number of member stars
$\rm N_*=282$, and a total mass of $\mbox{$\rm m_{MS+PMS}$}=435\,\mbox{$\rm M_\odot$}$.

The presence of significant numbers of PMS stars in NGC\,6611 has been confirmed by means of the
observation of a large number of emission-line stars and IR disk signatures (Hillenbrand et al.
\cite{Hillenbrand93}; Massey et al. \cite{Massey95}), which is an expected population in such a
young cluster. Recently Oliveira et al. (\cite{Oliveira05}) obtained IZJHKL' photometry aiming
at identifying PMS stars in NGC\,6611. Their Fig.~2 shows the CMDs $\rm I\times (I-Z)$ for the
central area ($\rm7\arcmin\times6\arcmin$) and for a control field 16\arcmin\ away from the cluster
center. The PMS population, defined within $\rm 12<I<19$, corresponding to the mass range $\rm
0.4<m(\mbox{$\rm M_\odot$})<7$, stands out in the central area and decreases significantly towards the control field.
The MS population does not show such trend, its spatial distribution remaining apparently constant
throughout the fields.

In the left panel of Fig.~\ref{fig1} we provide an R XDSS image encompassing an area of
$1^\circ\times1^\circ$ centered on NGC\,6611, extracted from the Canadian Astronomy Data Centre
(CADC\footnote{\em http://cadcwww.dao.nrc.ca/}). In the right panel we show the corresponding
2MASS J image. The stark contrast between the R and J images reflects primarily the effect of
the $\rm H\alpha$ emission in the R band and how dust is much more penetrable in the near-infrared
bands. Thus,
the analysis of NGC\,6611 and its outskirts with near-infrared data is naturally justified
because it allows access to low-mass stars with moderate aperture telescopes. In this sense,
Hillenbrand et al (\cite{Hillenbrand93}) investigated NGC\,6611 by means of deep near-infrared
observations covering a $15\arcmin\times15\arcmin$ area with useful limits of J=16, H=14.5 and
K=13.5, similar to those of 2MASS.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{2793fig2.eps}}
\caption[]{Spatial distribution of the number of stars (brighter than $\rm\mbox{$\rm J$}=15.8$) around the
central position of NGC\,6611. The density of stars increases to the East and South. $1\sigma$
Poisson errors are shown.}
\label{fig2}
\end{figure}

According to the WEBDA\footnote{\em http://obswww.unige.ch/webda} open cluster database
(Mermilliod \cite{Merm1996}), the central coordinates of NGC\,6611 are (J2000) $\alpha=18^h18^m48^s$,
and $\delta=-13^\circ48\arcmin24\arcsec$. However, the corresponding radial density profile
(Sect.~\ref{struc}) presented a dip for $\rm R=0\arcmin$. Accordingly, we searched for a new center
by examining histograms for the number of stars in 1\arcmin\ bins of right ascension and declination.
The resulting coordinates which maximize the density of stars at the center are (J2000) $\alpha=18^h18^m40.8^s$,
and $\delta=-13^\circ47\arcmin24.0\arcsec$, corresponding to $\ell=16.95^\circ$ and $b=0.83^\circ$.
In what follows we refer to these optimized coordinates as the center of NGC\,6611. WEBDA gives a
colour excess of $\mbox{$\rm E(B-V)$}=0.768$, distance to the Sun $\mbox{$\rm d_\odot$}=1.75$\,kpc, and $\rm age\approx7.6\,Myr$.

\section{Photometric parameters from 2MASS data}
\label{2mass}

The VizieR\footnote{\em http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246} tool was
used to extract \mbox{$\rm J$}, \mbox{$\rm H$}\ and \mbox{$\rm K_S$}\ 2MASS photometry of the stars present in a circular area
with radius $\rm R=60\arcmin$ centered on the optimized coordinates described in the previous
section. The faint-magnitude limit of the extracted stars is brigther than that corresponding
to the 99.9\% Point Source Catalogue Completeness Limit\footnote{According to the Level\,1
Requirement, according to
{\em\tiny http://www.ipac.caltech.edu/2mass/releases/allsky/doc/sec6\_5a1.html }}, $\mbox{$\rm J$}=15.8$,
$\mbox{$\rm H$}=15.1$\ and $\mbox{$\rm K_S$}=14.3$, respectively.

As a first step in the investigation of NGC\,6611 we use the 2MASS data to examine in Fig.~\ref{fig2}
the distribution of stars in the area surrounding the cluster. Each panel depicts the number of stars
brighter than $\rm\mbox{$\rm J$}=15.8$ in strips of 5\arcmin\ width in declination (left panels) and right
ascension (right panels) with respect to the optimized cluster center. The rather concentrated structure
of NGC\,6611 is apparent in panels (e) and (f). Within uncertainties the cluster appears to be spatially
asymmetric, being more extended in right ascension (apparent diameter $\rm D_\alpha\sim21\arcmin$,
(panel (e)) than in declination ($\rm D_\delta\sim12\arcmin$, (panel (f)). The spatial distribution of
stars around the cluster is non-uniform, increasing significantly above the $1\sigma$ Poisson errors
towards the East (panels (a), (c), (e) and (g)) and less markedly to the South (panels (b) and (d)).
Part of this non-uniformity can be accounted for by differential reddening, which is important
throughout the cluster area (Belikov et al. \cite{Belikov99}).

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{2793fig3.eps}}
\caption[]{$\mbox{$\rm J$}\times\mbox{$\rm (J-H)$}$ CMDs of the central 9\arcmin\ of NGC\,6611. Left panels: observed
photometry. Middle panels: reddening-corrected CMDs according to Belikov et al. (\cite{Belikov99}).
Right panels: reddening-corrected and field-star decontaminated CMDs. Note the extended MS and
conspicuous PMS population,
which is restricted essentially to the central 6\arcmin. Field stars are shown as x in the middle
panels. Filled circles in the bottom panels: O\,V stars from Bosch, Morrell \& Niemel\"a
(\cite{Bosch99}).}
\label{fig3}
\end{figure}

\subsection{Spatial variation of reddening}
\label{SVR}

Because of the low Galactic latitude ($b=0.83^\circ$), the field of NGC\,6611 presents significant
field-star contamination. This can be seen in the left panels of Fig.~\ref{fig3} where we show the
observed $\mbox{$\rm J$}\times\mbox{$\rm (J-H)$}$ CMDs of three consecutive circular regions ($\rm\Delta R=3\arcmin$)
centered on NGC\,6611. Besides conspicuous MS stars, the integrated CMD up to $\rm R=9\arcmin$ (bottom
panel) presents important field-star contamination.

As discussed in Belikov et al. (\cite{Belikov99}), the spatial field of NGC\,6611 is critically affected
by differential reddening with important variations both in \mbox{$\rm E(B-V)$}\ and $\rm R_V$ in areas separated
by distances as small as $\sim2\arcmin$. They present \mbox{$\rm E(B-V)$}\ and $\rm R_V$ values derived from spectroscopy
and proper motion of cluster stars in $\rm2\arcmin\times2\arcmin$ cells covering an area of about
$\rm40\arcmin\times36\arcmin$ centered on NGC\,6611. Note that \mbox{$\rm E(B-V)$}\ in each cell corresponds to
the absolute reddening value.

We applied the above procedure to produce reddening-corrected 2MASS photometry for all stars in each
cell to yield a total region reaching $\rm R\approx23\arcmin$ from the center of NGC\,6611. In the
vacant cells we followed their suggestion and adopted the average values of \mbox{$\rm E(B-V)$}\ and $\rm R_V$.  For
reddening and absorption transformations in the 2MASS bands we use the relations $\rm A_J=0.276\times
R_V\,\mbox{$\rm E(B-V)$}$, $\rm A_H=A_J-0.33\,\mbox{$\rm E(B-V)$}$ and $\rm A_{K_S}=A_J- 0.49\,\mbox{$\rm E(B-V)$}$, according to Dutra, Santiago
\& Bica (\cite{DSB2002}, and references therein).

The resulting reddening-corrected CMDs are shown in the middle panels of Fig.~\ref{fig3}. Comparison
of the reddening-corrected CMDs with the observed ones shows that the average colour-excess throughout
the cluster area is $\langle\mbox{$\rm E(J-H)$}\rangle=0.25$, corresponding to $\langle\mbox{$\rm E(B-V)$}\rangle=0.8$.

\subsection{Field-star decontamination}
\label{FSD}

Finally, to uncover the intrinsic CMD morphology we apply a field-star decontamination procedure.
Because of the spatial limitation on the useful area caused by the differential-reddening correction
(Sect.~\ref{SVR}), we consider as offset field the ring located at $\rm17\arcmin\leq R\leq22\arcmin$.
This area is large enough to produce statistical representativity of the field stars, both in magnitude
and colours.

To illustrate the amount and colour-magnitude distribution of the contamination in the area of NGC\,6611
we plot in the middle panels of Fig.~\ref{fig3} the corresponding (same area) field-star contributions
taken from rings with external radius at 22\arcmin. As a consequence we can see that most of the faint
stars - in particular those mimicking a low-MS - are in fact field-stars.

Based on the spatial number-density of stars in the offset field, the decontamination procedure estimates
the number of field stars which within the $\rm1\sigma$ Poisson fluctuation should be present in the
cluster field. The observed CMD is then divided in colour/magnitude cells from which stars are randomly
subtracted in a number consistent with the expected number of field stars in the same cell. The
dimensions of the colour/magnitude cells can be subsequently changed so that the total number of stars
subtracted throughout the wole cluster area matches the expected one, within the $\rm1\sigma$ Poisson
fluctuation. Since the field stars are taken from an external annulus of fixed dimensions, corrections
are made for the different solid angles of cluster and offset field. This procedure can be applied
to the cluster region as a whole or internal regions as well. Note that because this procedure actually
excludes stars from the original files - thus artificially changing both the radial distribution of stars
and the LF - we use it only for the sake of uncovering the intrinsic CMD morphology.

The resulting field-star decontaminated (differential-reddening corrected) CMDs are shown in the right
panels of Fig.~\ref{fig3}. As expected, most of the faint-star distribution was subtracted by the
decontamination procedure. The central region ($\rm0\arcmin\leq R\leq3\arcmin$) presents an extended,
vertical MS reaching from $\mbox{$\rm J$}\approx11.5$ to $\mbox{$\rm J$}\approx5.5$ which reflects the young age of NGC\,6611.
This region also presents a conspicuous population of PMS stars ($\rm0.54\leq\mbox{$\rm (J-H)$}\leq1.1$) which extends
essentially up to $\rm R\approx6\arcmin$. The entry point (turn-on stars) of the PMS into the MS occurs
at $\mbox{$\rm J$}\approx11.1$. The region $\rm6\arcmin\leq R\leq9\arcmin$\ is sparsely populated by cluster stars,
with a small fraction of MS and PMS stars still discernible.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{2793fig4.eps}}
\caption[]{$\rm\mbox{$\rm (H-K_S)$}\times\mbox{$\rm (J-H)$}$ diagram of the central 3\arcmin\ (Panel (a)) and 9\arcmin\ (Panel (b))
of NGC\,6611. Dashed line: 4\,Myr Padova isochrone. Dotted line: 1\,Myr sequence of PMS stars
(Siess, Dufour, \& Forestini \cite{Siess2000}).
Solid line: MS stars from Schmidt-Kaler (\cite{SK82}). Filled triangles: O\,V stars (Bosch, Morrell,
\& Niemel\"a \cite{Bosch99}). Filled circles: reddening vectors; $\rm\Delta\mbox{$\rm E(B-V)$}=0.25$ between 2
consecutive circles. The corresponding field stars are shown in Panel (a) as `x'. Both diagrams were
produced after field-star decontamination.}
\label{fig4}
\end{figure}

\subsection{Age}
\label{age}

Deriving a precise age for clusters younger than $\sim10$\,Myr by means of isochrone fit is a
difficult task because of the nearly-vertical MS and lack of post-MS stars. As a consequence of
the scarcity of observational constraints in the CMD, several age-solutions are possible. In the
case of NGC\,6611, the CMD (Fig.~\ref{fig3}) can be acceptably fitted with isochrones with ages up
to 10\,Myr. In the present case we use the set of solar-metallicity isochrones of Padova (Girardi
et al. \cite{Girardi2002}) computed with the 2MASS \mbox{$\rm J$}, \mbox{$\rm H$}\ and \mbox{$\rm K_S$}\ filters\footnote{\em\tiny
http://pleiadi.pd.astro.it/isoc\_photsys.01/isoc\_photsys.01.html}. The 2MASS transmission filters
produced isochrones very similar to the Johnson ones, with differences of at most 0.01 in \mbox{$\rm (J-H)$}\
(Bonatto, Bica \& Girardi \cite{BBG2004}).

On the other hand, properties of young/embedded objects, in particular the age, can be
alternatively inferred by means of infrared colour-colour diagrams (e.g. Lada, Alves \& Lada
\cite{LAL96}). The fraction of stars with \mbox{$\rm K_S$}\ excess in embedded clusters is an age indicator
(e.g. Lada, Alves \& Lada \cite{LAL96}; Soares \& Bica \cite{SB02}) in the sense that larger fractions
correspond to younger evolutionary stages. In Fig.~\ref{fig4} we show the $\rm\mbox{$\rm (H-K_S)$}\times\mbox{$\rm (J-H)$}$ diagram
of the central 3\arcmin\ (Panel (a)) and 9\arcmin\ (Panel (b)) of NGC\,6611. Both diagrams were
produced after differential-reddening correction and field-star decontamination. To compare stars
in different evolutionary stages we show in Panel (a) the loci occupied by MS stars according to the
youngest Padova isochrone (4\,Myr) and to those of Schmidt-Kaler (\cite{SK82}). The 1\,Myr sequence
of PMS stars (Siess, Dufour, \& Forestini \cite{Siess2000}), and the loci of the O\,V stars with
available spectroscopic data of Bosch, Morrell, \& Niemel\"a (\cite{Bosch99}) are shown as well.
Extinction effects can be estimated by the reddening vectors.

For NGC\,6611 we measured within $\rm R\leq3\arcmin$ a fraction of $\rm f_{exc}=0.54\pm0.05$ of
\mbox{$\rm K_S$}\ excess stars. Considering uncertainties this value is intermediate between those of the
$\rho$ Ophiuchi cluster ($\rm f_{exc}=0.5 - 0.7$ -- Greene \& Young \cite{GY92}; Strom, Kepner,
\& Strom \cite{Strom95}) with an age of 1\,Myr or less (Greene \& Meyer \cite{GM95}) and that of
the Taurus Dark Nebula group ($\rm f_{exc}=0.5$ -- Kenyon \& Hartmann \cite{KH95}) with an age of
1.5\,Myr. Based on this we estimate an age of $\rm1.3\pm0.3$\,Myr for NGC\,6611. These values are
similar to those of Trapezium, NGC\,2327 cluster and BRC\,27 cluster (Soares \& Bica \cite{SB02}).

This estimate is consistent with {\it (i)} the presence of a significant population
of PMS (e.g. Walker \cite{Walker61}; Hillenbrand et al. \cite{Hillenbrand93}; Massey et al.
\cite{Massey95}; Oliveira et al. \cite{Oliveira05}), {\it (ii)} the fraction of $\sim58\%$ of
PMS having circumstellar discs (e.g. Hillenbrand et al. \cite{Hillenbrand93}; Massey et al.
\cite{Massey95}; Oliveira et al. \cite{Oliveira05}), and {\it (iii)} the fact that NGC\,6611
is ionizing the \ion{H}{ii} region Sh2-49 (e.g. Bosch, Morrell, \& Niemel\"a \cite{Bosch99};
Hillenbrand et al. \cite{Hillenbrand93}).

\subsection{Distance from the Sun}
\label{dsun}

Similarly to the age, the lack of evolved features in the CMD of NGC\,6611 precludes a precise
distance determination based directly on isochrone fit. In this sense we will derive the distance
of NGC\,6611 from the Sun using two independent methods. Bosch, Morrell \& Niemel\"a (\cite{Bosch99})
derived spectroscopic data of 8 MS O member stars (which are identified in the bottom panels of
Fig.~\ref{fig3}). Each O\,V star was corrected for reddening according to the corresponding
cell \mbox{$\rm E(B-V)$}\ and $\rm R_V$ values in Belikov et al. (\cite{Belikov99}). From these stars we derive
an absolute average distance modulus of $\rm\mbox{$\rm (m-M)_O$}=11.39\pm0.46$, corresponding to a distance from
the Sun $\rm\mbox{$\rm d_\odot$}=1.92\pm0.45\,kpc$. We use this value to set the 4\,Myr Padova isochrone in the
reddening-corrected, field-star decontaminated CMD of the central 6\arcmin\ of NGC\,6611 in
Fig.~\ref{fig5}. Within uncertainties, the least-massive stars already in the MS of NGC\,6611 have
mass in the range 3--5\,\mbox{$\rm M_\odot$}.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{2793fig5.eps}}
\caption[]{The 4\,Myr Padova isochrone set to the reddening-corrected, field-star decontaminated
CMD of the central 6\arcmin\ of NGC\,6611 according to $\mbox{$\rm d_\odot$}=1.92\pm0.45$\,kpc. PMS model isochrones
of Siess, Dufour, \& Forestini (\cite{Siess2000}) with ages of 200\,Kyr, 1\,Myr and 4\,Myr are fitted
to the PMS population resulting in $\rm\mbox{$\rm d_\odot$}=1.65\pm0.27\,kpc$. Evolutionary tracks for PMS stars of
masses 1, 2, 3and 5\,\mbox{$\rm M_\odot$}\ are shown as dotted lines. }
\label{fig5}
\end{figure}

Alternatively, we estimate the distance of NGC\,6611 by means of the MS entry point of the PMS
stars. To do this we use the turn-on locus in the reddening-corrected, field-star decontaminated
CMD of the central 6\arcmin\ in Fig.~\ref{fig5}. The PMS stars in Fig.~\ref{fig5} turn out to be
basically contained within the 200\,Kyr and 4\,Myr isochrones (Siess, Dufour, \& Forestini
\cite{Siess2000}), after applying an absolute distance modulus of $\rm\mbox{$\rm (m-M)_O$}=11.09\pm0.30$.
This corresponds to a distance from the Sun of $\rm\mbox{$\rm d_\odot$}=1.65\pm0.27\,kpc$ which, within the
uncertainties, agrees with the previous value based on the O\,V stars. For completeness we also
show in Fig.~\ref{fig5} evolutionary tracks up to the zero-age main sequence (ZAMS) for PMS stars
with masses 1, 2, 3 and 5\,\mbox{$\rm M_\odot$}. Similarly to the value based on the 4\,Myr Padova isochrone, the
low-mass MS of NGC\,6611 implied by the PMS occurs in the range 3--5\,\mbox{$\rm M_\odot$}.

Based on the above estimates we adopt the average value $\rm\mbox{$\rm d_\odot$}=1.8\pm0.5\,kpc$ as the distance of
NGC\,6611 from the Sun. With this value the Galactocentric distance of NGC\,6611 turns out to be
$\mbox{$\rm d_{GC}$}=6.3\pm0.5$\,kpc, using 8.0\,kpc as the distance of the Sun to the center of the Galaxy (Reid
\cite{Reid93}). The present value of the distance from the Sun agrees with that derived by Tadross
et al. (\cite{Tad2002}) and is comparable to that of WEBDA (1.75\,kpc), but falls $\sim0.5$\,kpc
short with respect to the average value found in the literature.

\section{Cluster structure}
\label{struc}

Structural parameters of NGC\,6611 were derived by means of the radial density profile, defined as the
projected number of stars per area around the cluster center. In the case of this low-latitude cluster
the contamination of the CMD by field stars must be taken into account in order to derive the intrinsic
radial distribution of stars. We do this by considering the colour-magnitude filter shown in the inset
of Fig.~\ref{fig6} which, within uncertainties, describes the cluster CMD morphology from the upper MS
to the PMS stars. Before counting stars we applied the colour-magnitude filter to the differential-reddening
corrected CMD of the cluster (including stars with distance to the center from 0\arcmin\ to 23\arcmin), to
discard stars with discrepant colours. The colour-magnitude filtering procedure has been previously
applied in the analysis of the open clusters M\,67 (Bonatto \& Bica \cite{BB2003}), NGC\,188 (Bonatto,
Bica \& Santos Jr. \cite{BBS2004}) and NGC\,3680 (Bonatto, Bica \& Pavani \cite{BBP2004}). The radial
density profile was obtained by counting stars inside concentric annuli with a step of 0.5\arcmin\
in radius. In the present case the background contribution level corresponds to the average number
of stars included in the ring located at $\rm 17\arcmin\leq R\leq 22\arcmin$ ($\rm 8.8\leq
R(pc)\leq11.4$), resulting in $\rm\sigma_{bg}=2.14\pm0.06\,stars\,(\arcmin)^{-2}=
7.8\pm0.2\,stars\,pc^{-2}$. Note that the colour-magnitude filter encompasses both the MS
and PMS stars.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{2793fig6.eps}}
\caption[]{Radial density profile of the cluster NGC\,6611. Dashed line: 2-parameter King profile. Shaded
region: stellar background level (average number of stars in the ring $17\arcmin\leq R\leq22\arcmin$).
The dimension of the core is indicated. The colour-magnitude filter used to discard stars with discrepant
colours is shown in the inset, superimposed on the reddening-corrected and field-star decontaminated CMD
of the central 6\arcmin.}
\label{fig6}
\end{figure}

The resulting radial density profile of the $\rm MS + PMS$ stars is shown
in Fig.~\ref{fig6}. For absolute comparison between clusters we scale the radius in the abscissa
in parsecs, and the number density of stars in the ordinate in $\rm stars\,pc^{-2}$\ using the
distance derived in Sect.~\ref{2mass}. The statistical significance of the profile is reflected
in the $1\sigma$\ Poisson error bars.

Structural parameters of NGC\,6611 were derived by fitting the two-parameter King (\cite{King1966a})
surface density profile to the background-subtracted radial distribution of stars. The two-parameter
King model essentially describes the intermediate and central regions of normal clusters (King
\cite{King1966b}; Trager, King \& Djorgovski \cite{TKD95}). The fit was performed using a nonlinear
least-squares fit routine which uses the errors as weights. The best-fit solution is shown in
Fig.~\ref{fig6} superimposed on the observed radial density profile. Parameters derived are the King
background-subtracted central density of stars $\rm\sigma_{0K}=35\pm6\,stars\,(\arcmin)^{-2}=128\pm20
\,stars\,pc^{-2}$, and the core radius $\rm\mbox{$\rm R_{core}$}=1.35\pm0.15\arcmin=0.7\pm0.1\,pc$. Considering the
radial density profile fluctuations with respect to the background level, we can
define a limiting radius (\mbox{$\rm R_{lim}$}) for the cluster, in the sense that for regions beyond $\mbox{$\rm R_{lim}$}$, the
null-contrast between cluster and background star density would produce large Poisson
errors and consequently, meaningless results. Thus, for practical purposes, the
bulk of the cluster stars are contained within $\mbox{$\rm R_{lim}$}$. For NGC\,6611 we estimate a limiting radius
$\rm\mbox{$\rm R_{lim}$}=12.5\pm1.0\arcmin=6.5\pm0.5\,pc$.

Despite the young age of NGC\,6611 the King profile provides a good fit of the  stellar content
in this cluster, within uncertainties. Since it follows from an isothermal (virialized) sphere,
the close similarity of the radial distribution of stars in NGC\,6611 with a King profile may
suggest that the internal structure of this cluster (particularly the core) has reached some
level of energy equipartion. However, part of this effect appears to be related to formation
processes as well (Sects.~\ref{dyna} and \ref{comp}).

\section{Luminosity and mass functions of the MS}
\label{MF}

The rather populous nature of NGC\,6611 provides an opportunity to study the spatial distribution
of LFs and MFs $\left(\phi(m)=\frac{dN}{dm}\right)$ of the MS stars in such a young open cluster.

Based on the King profile fit of the MS radial density profile of NGC\,6611 (Fig.~\ref{fig6}) we
decided to study the MF in the following regions: {\em (i)} $\rm 0.0\leq R(pc)\leq0.7$ (core),
{\em (ii)} $\rm 0.7\leq R(pc)\leq6.5$ (halo), and {\em (iii)} $\rm 0.0\leq R(pc)\leq6.5$\ (overall).
In order to maximize the significance of background counts, we consider as offset field the
outermost ring at $\rm 8.8\leq R(pc)\leq 11.4$, which lies $\sim2.3$\,pc beyond the limiting
radius.

Similarly to the structural analysis (Sect.~\ref{struc}) the first step in the present analysis
is to take into account the field-star contamination. In this case we apply the colour-magnitude
filter (Fig.~\ref{fig6}) restricted to the MS stars (i.e. $\mbox{$\rm J$}\leq11.4$). The filtering process
takes into account most of the field stars, leaving only a residual contamination. We deal with
this residual contamination statistically by building LFs for each cluster region and offset field
($17\arcmin\leq R\leq22\arcmin$) separately. We consider the three 2MASS bands independently when
building the LFs. Note that the faint-magnitude limit of the MS is significantly brighter than that
of the 99.9\% Point Source Catalogue Completeness Limit (Sect.~\ref{2mass}). We take $\rm\mbox{$\rm J$}=5$ as
the upper-MS limit (Fig.~\ref{fig3}). We build the LF of each 2MASS band by counting stars in magnitude
bins from the respective faint magnitude limit to the upper MS, both for each cluster region and offset
field. Considering that the solid angle of the offset field may be different from that of a given
cluster region, we multiply the offset field LF by a numerical factor so that the solid angles match.
The intrinsic LF of each cluster region is obtained by subtracting the respective (i.e. solid angle-corrected)
offset field LF from that of the cluster region. Finally, the intrinsic LFs are transformed into MFs
using the mass-luminosity relation obtained from the 4\,Myr Padova isochrone (the youngest one available)
and the absolute distance modulus $\mbox{$\rm (m-M)_O$}=11.39$ (Sect.~\ref{2mass}). These procedures are repeated
independently for the three 2MASS bands. The final MF of a given cluster region is produced by
combining the \mbox{$\rm J$}, \mbox{$\rm H$}\ and \mbox{$\rm K_S$}\ MFs into a single MF. The resulting core, halo and overall MFs of
NGC\,6611, covering the mass range $\rm5\leq m(\mbox{$\rm M_\odot$})\leq25$, are shown in Fig.~\ref{fig7}.
To these MFs we fit the function $\phi(m)\propto m^{-(1+\chi)}$. The resulting fits are shown in
Fig.~\ref{fig7}, and the MF slopes are given in col.~4 of Table~\ref{tab2}.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{2793fig7.eps}}
\caption[]{Mass functions of the MS stars (empty circles) in different spatial regions of
NGC\,6611. Each panel contains MFs derived from the \mbox{$\rm J$}, \mbox{$\rm H$}\ and \mbox{$\rm K_S$}\ 2MASS photometry. MF
fits $\left(\phi(m)\propto m^{-(1+\chi)}\right)$ are shown as dashed lines, and the respective MF
slopes are given. The insets show the $\rm MS+PMS$ field-star subtracted LFs in each spatial region.}
\label{fig7}
\end{figure}

We show in each panel of Fig.~\ref{fig7} the corresponding field-star subtracted LFs, where the
relative contribution of the PMS ($\rm M_J\geq-0.12$) with respect to the MS can be evaluated.

Both the overall and halo MFs are slightly steeper than a typical Salpeter (\cite{Salpeter55}) IMF
($\chi=1.35$); however, the core MF turned out to be flat, with $\chi=0.62\pm0.16$. The difference in
MF slope between the core and halo ($\chi=1.52\pm0.13$, panel (b) of Fig.~\ref{fig7}), may be a
consequence of mass segregation in the core. We discuss this point further in Sect.~\ref{dyna}.

\subsection{Total observed mass}
\label{TM}

We provide in Table~\ref{tab2} parameters derived from the MFs of each spatial region considered.
The number of PMS stars in the core, halo and overall regions was estimated upon integration
of the respective field star-subtracted LFs (Fig.~\ref{fig7}) for $\rm M_J\geq-0.12$.
Considering the observed distribution of PMS stars and the respective evolutionary tracks
(Fig.~\ref{fig5}) and the fact that MFs in general increase in number for the subsolar-mass
range, for simplicity we assume an average PMS mass of 1\,\mbox{$\rm M_\odot$}. The resulting number and mass of
PMS stars are in cols.~2 and 3, respectively The observed number of MS stars and corresponding
mass (cols.~5 and 6,
respectively) are derived by integrating the MF through the mass range 5--25\,\mbox{$\rm M_\odot$}. We add to
these the corresponding values of the number and mass of PMS stars to derive the total number of
observed stars (col.~7), observed mass (col.~8), projected mass density (col.~9) and mass density
(col.~10).

\begin{table*}
\caption[]{Parameters derived from the MFs and PMS stars.}
\label{tab2}
\renewcommand{\tabcolsep}{0.7mm}
\renewcommand{\arraystretch}{1.6}
\begin{tabular}{cccccccccccccccc}
\hline\hline
&\multicolumn{2}{c}{PMS}&&\multicolumn{4}{c}{Observed MS}&
&\multicolumn{4}{c}{$\rm Observed\ MS+PMS$}&&$\tau$\\
\cline{2-3}\cline{5-8}\cline{10-13}\\
Region&N$^*$&m &&$\chi_{5-25}$&&$\rm N^*$&\mbox{$\rm m_{obs}$}&&$\rm N^*$&\mbox{$\rm m_{MS+PMS}$}&$\sigma$&$\rho$\\
(pc)&($10^2$stars)&($10^2\mbox{$\rm M_\odot$}$)& &&&($10^2$stars)&($10^2\mbox{$\rm M_\odot$}$)&& ($10^2$stars)&
($10^2\mbox{$\rm M_\odot$}$)&($\rm \mbox{$\rm M_\odot$}\,pc^{-2}$)&($\rm \mbox{$\rm M_\odot$}\,pc^{-3}$)\\
 (1)& (2) & (3) && (4) &&(5) &(6) && (7)& (8) & (9) & (10)&&(11)\\
\hline
Core&$1.0\pm0.3$&$1.0\pm0.3$&&$0.62\pm0.16$& &$0.3\pm0.2$&$2.3\pm1.3$
&&$1.2\pm0.4$&$4.1\pm1.6$&$265\pm107$&$284\pm115$&&$1.8\pm0.6$\\

Halo&$2.6\pm0.8$&$2.6\pm0.8$ &&$1.52\pm0.13$& &$0.8\pm0.3$&$6.9\pm2.9$
 &&$3.4\pm0.9$&$9.6\pm3.1$&$7.3\pm2.3$&$0.83\pm0.27$&&---\\

Overall&$3.6\pm1.2$&$3.6\pm1.2$ &&$1.45\pm0.13$& &$0.9\pm0.3$&$8.4\pm3.2$
&&$4.5\pm1.2$&$12.0\pm3.4$&$9.0\pm2.6$&$1.0\pm0.3$&&$0.067\pm0.022$\\

\hline
Overall$^\dag$&$3.6\pm1.2$&$3.6\pm1.2$ &&$1.45\pm0.13$& &$1.0\pm0.3$&$12.7\pm3.5$ &&$4.6\pm1.3$&$16.3\pm3.5$&$12.3\pm2.6$&$1.4\pm0.3$&&$0.066\pm0.022$\\
\hline\hline
\end{tabular}
\begin{list}{Table Notes.}
\item Observed mass range: $\rm5-25\,\mbox{$\rm M_\odot$}$. Col.~4 gives the MF slope derived for the MS stars.
Col.~11: dynamical-evolution parameter $\rm\tau=age/t_{relax}$. ($\dag$): includes stars more
massive than 25\,\mbox{$\rm M_\odot$}.
\end{list}
\end{table*}

To complete the census of the mass stored in observed stars in NGC\,6611 we must include
as well the stars more massive than 25\,\mbox{$\rm M_\odot$}, which although present in the photometry, have not been
counted in the mass estimate owing to the adopted MF upper cutoff ($\rm25\,\mbox{$\rm M_\odot$}$). Hillenbrand et al.
(\cite{Hillenbrand93}) give the number of stars in
selected mass bins for massive stars: 5 stars with mass in the range $\rm
25\leq m(\mbox{$\rm M_\odot$})\leq40$, 4 with $\rm 40\leq m(\mbox{$\rm M_\odot$})\leq60$, and 1 with $\rm 60\leq m(\mbox{$\rm M_\odot$})\leq85$.
Accordingly, the mass stored in stars more massive than 25\,\mbox{$\rm M_\odot$}\ amounts to $\approx435\,\mbox{$\rm M_\odot$}$,
about 50\% of the mass implied by the MF of the main sequence range considered above
(col.~6 of Table~\ref{tab2}). For simplicity we add their mass to the overall region. To this
effect we include an additional entry in Table~\ref{tab2} to account for the massive stars,
resulting in $\rm\mbox{$\rm m_{MS+PMS}$}\sim1630\,\mbox{$\rm M_\odot$}$. This value is $\sim4$\ times larger than the estimate of
Tadross et al. (\cite{Tad2002}). The total observed mass of NGC\,6611 is a factor $\approx2$ larger than
the mass estimated for the Trapezium cluster (Lada \& Lada \cite{LL2003}). It should be noted
that the above mass and density estimates (cols.~(8) - (10) in Table~\ref{tab2}) are in fact lower limits,
since we are not taking into account stars less massive than 5\,\mbox{$\rm M_\odot$}, a mass range for which we have no
information on the behaviour of the MF slope.

\subsection{Dynamical state of NGC\,6611}
\label{dyna}

The overall MF slope ($\chi=1.45\pm0.12$) in the mass range $\rm 5\leq m(\mbox{$\rm M_\odot$})\leq 25$ is similar
to that of a standard Salpeter ($\chi=1.35$) IMF. Besides, the MF slope presents large
variations in the inner regions, being flat ($\chi=0.62\pm0.16$) in the core and rather steep
($\chi=1.52\pm0.13$) in the halo (Table~\ref{tab2} and Fig.~\ref{fig7}). In older clusters
this fact reflects the effects of large-scale mass segregation, in the sense that low-mass stars
originally in the core are transferred to the cluster's outskirts while massive stars accumulate
in the core. This produces a flat MF in the core and a steep one in the halo (see, e.g. Bonatto
\& Bica \cite{BB2005}).

Mass segregation in a star cluster scales with the relaxation time, defined as $\rm
\mbox{$\rm t_{relax}$}=\frac{N}{8\ln N}\mbox{$\rm t_{cross}$}$, where $\rm\mbox{$\rm t_{cross}$}=R/\sigma_v$ is the crossing time, N is the (total) number
of stars and $\rm\sigma_v$\ is the velocity dispersion (Binney \& Tremaine \cite{BinTre1987}).
The characteristic time scale in which a cluster reaches some level of kinetic energy equipartition
is described by $\mbox{$\rm t_{relax}$}$, when massive stars sink to the core and low-mass stars are transferred to
the halo. Assuming a typical $\rm\sigma_v\approx3\,\mbox{$\rm km\,s^{-1}$}$ (Binney \& Merrifield \cite{Binney1998})
we obtain for the overall cluster $\rm\mbox{$\rm t_{relax}$}\sim20\pm5$\,Myr, and for the core $\rm\mbox{$\rm t_{relax}$}\sim0.7\pm0.2$\,Myr.
Considering that NGC\,6611 is $\sim1.3$\,Myr old (Sect.~\ref{2mass}), the age of this cluster is $\sim2$
times larger than $\rm\mbox{$\rm t_{relax}$}(core)$. Thus, the presence of mass segregation and consequently some
degree of MF slope flattening can be expected in the core. However, the ratio cluster age to
\mbox{$\rm t_{relax}$}\ drops to $\sim0.07$ for the overall cluster, which is consistent with the typical Salpeter
slope and the absence of important mass segregation.

Although OB stars in NGC\,6611 host more companions (for binaries with mass ratios $\rm q\geq0.1$)
than solar-type field stars (Duch\^ene et al. \cite{Duch2001}), the expected influence of binaries
in the MF would be to steepen the slope of a standard Salpeter IMF to $\chi\approx1.7$, and not to
flatten it out (Sagar \& Richtler \cite{SagRich91}; Kroupa \cite{Kroupa2004}).

\section{Comparison with clusters in different dynamical-evolution states}
\label{comp}

In the previous sections we derived a series of parameters related to the structure and
dynamical evolution of NGC\,6611. At this point it may be useful to check how this young
cluster fits in the context of open clusters with different ages and in more advanced
dynamical states. Bonatto \& Bica (\cite{BB2005}) presented a systematic analysis of a
set of open clusters with ages in the range 70 - 7\,000\,Myr and masses from 400 -
5\,300\,\mbox{$\rm M_\odot$}. The methodology used follows the same lines as that used the present paper.
As a result, a set of uniform parameters related to the structure (core and overall radii, mass
and density), dynamical state (core and overall MF slopes, evolutionary parameter $\rm\tau=age/\mbox{$\rm t_{relax}$}$),
as well as age and Galactocentric distance of open clusters was obtained. Some correlations
among these parameters were verified, and a separation of massive ($m\geq1\,000\,\mbox{$\rm M_\odot$}$) and
less-massive ($m\leq1\,000\,\mbox{$\rm M_\odot$}$) clusters was observed. The core and overall dynamical-evolutionary
parameter of NGC\,6611 is given in col.~11 of Table~\ref{tab2}.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{2793fig8.eps}}
\caption[]{Relations involving structural parameters of open clusters. Filled circles:
clusters more massive than 1\,000\,\mbox{$\rm M_\odot$}. Open circles, $\rm m<1\,000\,\mbox{$\rm M_\odot$}$. Filled triangle:
NGC\,6611. Dashed lines: least-squares fits to the nearby clusters (see text). Shaded areas:
$\rm1\sigma$ borders of the least-squares fits. Arrows indicate lower-limit estimates
of mass and density for NGC\,6611.}
\label{fig8}
\end{figure}

In Fig.~\ref{fig8} we compare NGC\,6611 with the set of nearby, well-studied older clusters
(Bonatto \& Bica \cite{BB2005}) in terms of structural parameters. Note that the
mass and density values of NGC\,6611 are lower limits (Sect.~\ref{TM}).
The limiting radius of NGC\,6611 fits in the low-limit correlation of \mbox{$\rm R_{lim}$}\ with age
(panel (d)). Although with a larger scatter, the same is observed in the correlation of \mbox{$\rm R_{core}$}\
with age (panel (g)). The core density of NGC\,6611 follows the trend presented by massive
clusters for young ages (panel (a)). A similar trend is seen for the overall density (panel (h)).
In Galactocentric distance the limiting radius of NGC\,6611 helps defining
a correlation (panel (b)) in the sense that clusters at larger \mbox{$\rm d_{GC}$}\ tend to be larger, which
agrees with the results of Lyng\aa\ (\cite{Lynga82}) and Tadross et al. (\cite{Tad2002}).
The large scatter in panel (e) precludes any conclusion with respect to a dependence of the core
radius with \mbox{$\rm d_{GC}$}. NGC\,6611 fits well in the tight correlations of core and overall mass (panel (i);
least-squares fit: $\rm M_{core}=(14.71\pm10.30)+(0.08\pm0.01)M_{overall}$ with a correlation
coefficient $\rm CC=0.92$),
and core and limiting radii (panel (f); $\rm \mbox{$\rm R_{lim}$}=(1.05\pm0.45)+(7.73\pm0.66)\mbox{$\rm R_{core}$}$ with
$\rm CC=0.95$). Finally, in Bonatto, \& Bica (\cite{BB2005}) we observed
that massive and less-massive clusters follow parallel, different paths in the plane
$\rm core\ radius \times overall\ mass$. NGC\,6611 consistently fits in the
the massive clusters path (panel (c)).

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{2793fig9.eps}}
\caption[]{Relations involving evolutionary parameters of open clusters. Symbols as in
Fig.~\ref{fig8}}
\label{fig9}
\end{figure}

NGC\,6611 is compared to older clusters in terms of dynamical-evolution related parameters in
Fig.~\ref{fig9}. NGC\,6611 fits in the tight correlations of core and overall MF slopes (panel (d); $\rm\chi_{core}=(-2.07\pm0.46)+(1.74\pm0.35)\times\chi_{overall}$, with $\rm CC=0.87$), and core
and overall evolutionary parameters (panel (c); $\rm\tau_{core}=(63.3\pm9.6)\times\tau_{overall}$,
with $\rm CC=0.91$). The young age and small Galactocentric distance of NGC\,6611 suggests
a correlation of \mbox{$\rm d_{GC}$}\ with age (panel (g)), which would agree with the result of Lyng\aa\
(\cite{Lynga82}). However, we note that this trend is mostly based on a single point (NGC\,6611)
and thus, a larger cluster sample within the central sector is necessary to establish the statistical
signficance of the correlation.
The Salpeter-like overall MF slope of NC\,6611 is consistent with the overall mass and age relation
when compared to other massive clusters (panels (a) and (i), respectively). The scatter in
panel (h) does not allow inferences on the relation of core MF slope with mass.
Finally, with respect to the evolutionary parameters of NGC\,6611, the overall MF slope (panel (b);
$\rm\chi_{overall}=(1.5\pm0.1)-(1.9\pm0.6)
\exp{-\left(\frac{16.3\pm13.1}{\tau_{overall}}\right)}$, with $\rm CC=0.89$)
follows the relations suggested by massive clusters with small values of $\tau$.
However, the core MF slope is flatter than that expected for its value of $\tau$ (panel (e);
$\rm\chi_{core}=(1.17\pm0.23)-(3.0\pm0.7)
\exp{-\left(\frac{439\pm156}{\tau_{core}}\right)}$, with $\rm CC=0.82$)
and age (panel (f)).

We conclude that both structurally and dynamically, the overall parameters of NGC\,6611
fit in the relations defined by older, more-massive open clusters,
in the loci expected of a very young cluster.

The core of NGC\,6611 presents a MF significantly flatter than that in
the halo, a situation typical of older clusters with important mass segregation. Part of this effect
can be accounted for by the fact that the core relaxation time is about half the cluster age.

\section{Concluding remarks}
\label{Conclu}

In this paper we analyzed the structure and mass distribution of MS and PMS stars in the ionizing
open cluster NGC\,6611. The analysis was based mostly on \mbox{$\rm J$}, \mbox{$\rm H$}\ and \mbox{$\rm K_S$}\ 2MASS photometry corrected
for the variable reddening across the region, from which we built radial density profiles and mass
functions. The average colour excess in a region reaching $\rm R\approx23\arcmin$ from the center of
NGC\,6611 resulted in $\mbox{$\rm E(J-H)$}=0.25$, corresponding to $\mbox{$\rm E(B-V)$}=0.8$. To uncover the intrinsic CMD morphology
we applied a field-star decontamination procedure to the reddening-corrected data. The resulting CMDs
present a MS restricted to stars more massive than $\approx5\,\mbox{$\rm M_\odot$}$ and a collection of PMS stars.

Based on the fraction of stars with \mbox{$\rm K_S$}\ excess we estimated an age of $\sim1.3\pm0.3$\,Myr for
NGC\,6611. We derived a distance from the Sun of $\rm\mbox{$\rm d_\odot$}=1.8\pm0.5\,kpc$, considering the values
calculated from O\,V stars with previous spectroscopic data and PMS tracks. Our value of \mbox{$\rm d_\odot$}\ agrees
with those given by Tadross (\cite{Tad2002}) and WEBDA. However, it locates NGC\,6611 $\sim0.5$\,kpc
closer to the Sun than the average value given in previous works. The direct method of distance
determination using stars is fundamental for the definition of the Galactic structure. Note that
available kinematic distances of the related \ion{H}{ii} region Sh2-49 are $\mbox{$\rm d_\odot$}=2.95$\,kpc (Georgelin,
\& Georgelin \cite{GG70}) and $\mbox{$\rm d_\odot$}=2.2$\,kpc (Blitz, Fich, \& Stark \cite{BFS82}), thus larger than
the present value.

King model fits to the radial density profiles including MS and PMS stars produced a core radius
$\mbox{$\rm R_{core}$}=0.70\pm0.08$\,pc with a limiting radius $\mbox{$\rm R_{lim}$}\approx6.5\pm0.5$\,pc. The projected density of
stars in the cluster center is $\rm\sim128\pm20\,stars\,pc^{-2}$.

Considering the field star-subtracted LFs, we estimated that the number of PMS stars in NGC\,6611 is
$\sim362$. The total observed mass locked up in PMS and MS stars amounts to
$\rm\mbox{$\rm m_{MS+PMS}$}=(1.6\pm0.3)\times10^3\,\mbox{$\rm M_\odot$}$. This is a lower-limit estimate since we are not
taking into account stars less massive than 5\,\mbox{$\rm M_\odot$}.

The core MF of the MS stars in NGC\,6611 is flat with a slope $\rm\chi=0.62\pm0.16$, while in the
halo it steepens to $\rm\chi=1.52\pm0.13$. The overall MF of NGC\,6611 is similar to a Salpeter
IMF with $\rm\chi=1.45\pm0.12$.

Compared to older open clusters in terms of structural and dynamical-evolution-related parameters,
the overall cluster behaves as a massive open cluster at young ages.

The spatial variation of MF slopes, being flat in the core and steeper in the halo, implies that
mass segregation has already affected the mass distribution in the core, since the relaxation time
$\rm\mbox{$\rm t_{relax}$}(core)\sim0.73$\,Myr corresponds to $\sim50\%$ of the cluster age. For the whole cluster $\rm\mbox{$\rm t_{relax}$}(overall)\sim20\,Myr\sim15\times\,$cluster age, which means that mass segregation did not
have time to redistribute stars in large scale throughout the body of such a young cluster.
Accordingly, the flattening degree in the core MF of NGC\,6611 seems to be related as well to
initial conditions, probably associated to the fragmentation of the parent molecular cloud itself,
with more massive proto-stars preferentially located in the central  parts of the cloud. This agrees
with Kroupa (\cite{Kroupa2004}) with respect to the observed degree of mass segregation in
clusters younger than a few Myr.

\begin{acknowledgements}
We are grateful to an anonymous referee for important remarks.
This publication makes use of data products from the Two Micron All Sky Survey, which
is a joint project of the University of Massachusetts and the Infrared Processing and
Analysis Center/California Institute of Technology, funded by the National Aeronautics
and Space Administration and the National Science Foundation. We also made use of the
WEBDA open cluster database. We acknowledge support from the Brazilian Institutions CNPq
and FAPEMIG.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


Sir William Johnson, Superintendent of Indian Affairs for the British, promised a substantial amount of Native warriors for the campaign to invade Canada, but fell short of his promise in the months leading up to the attack on Carrillon. The 450 warriors who joined him came from mostly the Iroquois, the Delaware, and the Choctaw. In general, the dress and appearance of these native warriors did not vary greatly, excepting the decorative details of their dress. Common in most articles of natives attire was their use of English goods and items of clothing. Their use of English goods reflected their relationship with Sir William Johnson as a trader, diplomat, and soldier. Johnson, a master at his job, went as far to marry in to the Mohawk tribe to seal these relationships. The attire of the native warriors speaks directly to Johnson's hard work.
Prisoner of the Delaware, John M'Cullough, described in his narrative what a native wore in 1756. Remarkably, he described many items that show up on Sir William Johnson's list of goods to purchase.
He had a brown coat on him, no shirt, his breast bare, a breech-clout, a pair of leggins and moccasons--his face and breast painted rudely with vermillion and vergigrease--a bunch of artificial hair, dyed of a crimson color, fixed on the top or crown of his head, a large triangle piece or silver hanging below his nose, that covered almost the whole of his upper lip; his ears were stretched out with fine brass wire.
Apart from the ornate decorations natives included in their attire being different from tribe to tribe,M'Cullough described generally the appearance of warriors with Sir William Johnson. M'Cullough also described the Native as being painted. Native warriors painted themselves from head to toe using bear grease mixed with colored pigments. These pigments also showed up amongst Sir William Johnson's list of trade goods with requests to purchase, "casks of vermillion," and, "lumps of verdegreace."
Johnson's list of arms was indicative of the relationship between the British and the Natives. He did not have a general request of arms; rather he was very specific in keeping with exactly what the natives requested. With intimate knowledge of the functioning of the native affairs, Johnson knew that failure to fulfill native requests could loose their support for the crown. Meeting demands for arms and trade goods, winning them over for the campaign Johnson brought with him 450 very well-equipped warriors to the campaign agains Fort Carillon. Having the basics to survive, the weapons to deliver a powerful blow to the enemy, and the paint and fineries to psychologically affect the enemy. As M'Cullough described one warrior, "he appeared something like what you might apprehend to be a likeness of the devil."
Best: Wool stroud cloth, decorated or undecorated.
Best: Well fit, unadorned or adorned wool Indian leggings, with hand woven garters.
Acceptable: Well fit, unadorned or adorned leather Indian leggings with hand woven garters.
Unacceptable: Gaiters, or baggy wool leggings.
Unacceptable: Officer's boots, half boots or; Dyer, Arrow, Minnetonka moccasins,Shoepacks.
Best: Hand-stitched white linen or correct period cotton shirt with narrow band cuffs with thread buttons or made for sleeve buttons (cuff links).
Acceptable: White linen or correct period cotton shirt with narrow band cuffs with thread buttons or made for sleeve buttons (cuff links) with minor visible machine-stitching.
Discouraged: Checked, striped linen, or wool shirts.
Best: Silk, linen, cotton neckerchief, sterling silver gorget, or shell gorget.
Best: English trade guns, English fowlers.
Acceptable: French trade guns, Fusil de Chasse.
Unacceptable: Blunderbuss, "blanket guns," cut down guns.
Best: Neck-knives, or sheathed trade knife; Hatchet, a curved sword, all carried on a simple leather belt or a sash.
Best: Quilled shot bag, and quilled slit pouch.
Discouraged: Plain shot bag, and plain slit pouch.
Unacceptable: Cartridge pouches and boxes, belly boxes.
Best: Native influenced horns reflecting Iroquois culture.
Acceptable: Plain white powder horn slung on a small leather strap.
Acceptable: Hemp tumpline, moose hair embroidered or plain.
Unacceptable: Two-strap knapsacks, snapsacks, French haversacks.
Acceptable: 2-3 point check, Dutch, or rose blankets. Sewn Skin robes, and bear skin hides may also be used.
Discouraged: Plain white or Hudson Bay blankets.
Best: Gourd canteen slung over the shoulder on a hemp cord or leather thong.
Acceptable: Glass or ceramic canteen, slung over the shoulder on a hemp cord or leather thong.
Discouraged: Leather or tin kidney shaped style canteen.


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This entry was posted in Uncategorized and tagged Duncan Clark, Engineering, News, scottish engineering on October 29, 2014 by Escape Recruitment Services.
Can it be learned or are "the best" just naturals?
I had a healthy discussion with my colleague this morning about an article in The Times looking at Bubba Watson's triumph in the US Masters in which the journalist praised the fact that Bubba is "self – taught" and had "never had a golf lesson in his life". The article concentrated on the fact that no one had shown him how to grip the club, control his swing or moulded him with their ideas rather than his own.
This entry was posted in Uncategorized and tagged personality on April 12, 2012 by Paul Leishman.


K-12 schools are subject to the Individuals with Disabilities Education Act (IDEA), Section 504 of the Rehabilitation Act, and the Americans with Disabilities Act (ADA). Post-secondary schools, however, are not subject to IDEA.
The IDEA is an entitlement statute that is about providing a free appropriate public education and enabling success in K-12.
On the other hand, Section 504 and the ADA are about equal access, the opportunity to compete. Both are civil rights laws to prevent discrimination. They apply in any setting (Section 504 only when an organization receives federal funding). Though Section 504 applies in K-12 settings, the application of Section 504 differs in post-secondary settings in that the emphasis is on equal opportunity to compete, not on succeeding or the position of a free public education (FAPE).
The definition of disability differs in post-secondary education. While the IDEA lists specific categories of disability, disability under Section 504 and the ADA is defined only as a significant limitation to a life function (such as hearing, speaking, breathing, walking, seeing, performing manual tasks, caring for oneself, working or learning). Therefore, it may be that a student who was eligible for special education services in a K-12 setting may not be eligible for disability services in a post-secondary setting, and a student needing services in the post-secondary setting would not have received special education in a K-12 setting.
For example, students having behavioral problems that cause learning disabilities might be eligible for special education in K-12, but they may not qualify for disability services or accommodation in a post-secondary setting. Students in wheelchairs could be considered eligible for accommodations in a post-secondary setting even if they never received special education during K-12 because they didn't need it.
In the post-secondary setting, students must be "eligible" for disability services under Section 504 and IDEA. They must be "otherwise qualified" for the educational program and meet eligibility standards for disability assistance. In the post-secondary setting, the laws are about access, not success.
Because the IDEA is an entitlement statue, in K-12 schools, it is the school's responsibility to identify children with disabilities and provide appropriate services to help them achieve a free appropriate public education. However, at the post-secondary level, it is the student's responsibility to "self-identify" in order to receive services. Indeed, the student must request services each semester s/he is enrolled in the institution if s/he desires services. If the student does not request services, no services will be provided. The post-secondary institution does not come to the student as in K-12 and does not provide an individualized education program (IEP) similar to those received in high school.
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These colorful Pineapple Core Slices are a fun snack for lunchboxes, and also are perfect for baking - easily adding fresh, tropical taste to cookies, cakes, pies and more. Colors include: yellow, orange, red, and green.
Pineapple Core, Sugar, Citric Acid, Sodium Metabisulphite (as SO2), FD&C Yellow 5, FD&C Red 40, FD &C Blue 1, FD&C Yellow 6, Lemon Flavor, Strawberry Flavor, Cantaloupe Flavor, Mango Flavor.


This post is a special treat for all you history buffs out there. The following collection of videos tells the story of one of the worst civil wars of modern European history — a war which also served as a testing ground for the biggest, bloodiest global conflict of all human history.
Filmed in the aftermath of Franco's death and featuring an impressive collection of first-hand accounts from people who fought on both sides of the conflict — nationalists, royalists, falangists, carlists, communists, syndicalists and anarchists, as well as members of the international brigades and the German and Italian armed forces — the documentary series is, to my mind, the most exhaustive audiovisual account that exists of the tragic events that befell Spain in the mid to late 1930s.


text:
Abergele ist eine Küstenstadt im County Borough Conwy County Borough im Norden von Wales (Großbritannien) zwischen Colwyn Bay und Rhyl.

Direkt vor der Küste befindet sich in etwa 8 Kilometer Entfernung der Windpark Rhyl Flats.

Traurige Berühmtheit errang der Ort, in dem auch noch eine Eisenkirche existiert, durch den Eisenbahnunfall von Abergele 1868.

Persönlichkeiten
Aylward Manley Blackman (1883–1956), Ägyptologe
Becky Brewerton (* 1982), Golferin
Justin Broadrick (* 1969), Musiker
Ralph Steadman (* 1936), Cartoonist
David Vaughan (* 1983), Fußballspieler
George Wynn (1886–1966), Fußballspieler

Weblinks

Ort in Conwy County Borough
Community im Conwy County Borough

redpajama_set_name: RedPajamaWikipedia


Hey toddlers! We're hosting a very special Moana themed Toddler Time featuring Sky-rannosaurus Rex! Toddlers 5 and under as well as their parents/caregivers can come by to meet Moana and Sky-Rannosaurus Rex on Saturday, May 11th at 9am! Only $10 per jumper will get you an hour of jump time and endless photo opportunities & memories! Limited space available!
No charge to non-jumpers accompanying toddlers. SkySocks sold separately. All jumpers required to have valid waiver on file and SkySocks. Passes (Annual Pass, 90-Day Pass, Super Pass, Toddler Pass, etc.) not valid during special Toddler Time.


text:
Q: Ember.js - this.set() in ApplicationRoute not working I am trying to set a boolean variable whenever the user is logged in.
App.ApplicationRoute = Ember.Route.extend({
  isLoggedIn: false,

  init: function() {
      if (loggedIn) {
        this.set('isLoggedIn', true);
      } else {
        console.log(error)
        this.set('isLoggedIn', false);
      }
    });
  }
});

However, on this.set() I get:

Uncaught TypeError: undefined is not a function

Any ideas?
I figured that the best place to handle user session is in the App.ApplicationRoute since its the root of everything. Does this cause a problem?
UPDATED:
With feedback here is the current / full code.
App.ApplicationRoute = Ember.Route.extend({
  isLoggedIn: false,

  init: function() {
    this._super();

    auth = new FirebaseSimpleLogin(appRef, function(error, user) {
      if (user) {
        console.log(user)
        this.set('isLoggedIn', true);
      } else {
        console.log(error)
        this.set('isLoggedIn', false);
      }
    });
  }
})

So I left out my Firebase code previously because I didnt really think it relevant, but for the sake of tracking down the problem, I'll add it in.

A: The reason has to do with the
this

being wrongly set in your firebasesimplelogin. The function you are using inside the constructor must be passed in a reference to 'this' of the outer context. The easiest way to do it is by changing the code of the function to this:
function(error, user) {
  if (user) {
    console.log(user)
    this.set('isLoggedIn', true);
  } else {
    console.log(error)
    this.set('isLoggedIn', false);
  }
}.bind(this));

A: First thing's first :)
As stated at the Ember.js documenation:

NOTE: If you do override init for a framework class like Ember.View or Ember.ArrayController, be sure to call this._super() in your init declaration! If you don't, Ember may not have an opportunity to do important setup work, and you'll see strange behavior in your application.

Second, your loggedIn variable is not declared nor instantiated and therefore null as well as your error but I guess you just ripped out some code of your project to fiddle together a quick example, so if you do:
App.ApplicationRoute = Ember.Route.extend({
  isLoggedIn: false,

  init: function() {
      this._super(); // <-- call `this._super()` here

      if (loggedIn) {
        this.set('isLoggedIn', true);
      } else {
        console.log(error)
        this.set('isLoggedIn', false);
      }
    });
  }
});

everything should work as expected :)


text:
Le cotre (de l'anglais cutter) est un voilier à un mât gréé en voile aurique à plusieurs focs, rapide et maniable, généralement équipé d'une grand-voile à corne, d'un flèche et de deux focs : le foc sensu stricto et la trinquette.

Détail du gréement

La bôme située en bas du mât supporte la grand-voile ; le foc et la trinquette sont en avant du mât. Dans les gréements traditionnels, la grand-voile est à corne ("cotre à corne") et le foc est amuré à un bout-dehors parfois très long.

Les voiliers modernes ont un système de voiles bermudiennes épurées et présentent seulement trois voiles : la grand-voile, le foc et la trinquette.

Le principal avantage du cotre était la division des voiles d'avant (focs) et donc leur surface, ce qui permettait une manipulation plus facile. La généralisation des enrouleurs de génois a quelque peu enlevé de l'intérêt à ce type de gréement sur les bateaux de plaisance actuels.

Utilisation historique

Usage civil
Leur gréement, présentant une surface de voile importante par rapport au gabarit (mât pouvant atteindre une trentaine de mètres), en particulier grâce à leurs multiples voiles d'avant (focs), leur donnait d'excellentes qualités de vitesse et de manœuvrabilité, avec en particulier une capacité à remonter au vent bien meilleure que les navires à voiles carrées. Ils étaient très utilisés comme :
 navire de pêche ; les termes sloop et cotre étaient à cette époque synonymes chez les pêcheurs ;
 navire de cabotage (pour les plus gros modèles) ;
 bateaux pilotes dans les ports comme au Havre ; on appelait ces cotres . Les cotres étaient aussi utilisés pour des missions de liaison et de surveillance côtière. Pour cette raison, les marines britannique et américaine continuent à appeler cutters leurs garde-côtes.

Usage militaire
Au temps de la marine à voile, les cotres étaient les plus petites unités des flottes militaires utilisées comme navire de guerre (corsaire par exemple) et appelé alors  (sloop-of-war). Ils étaient équipés de six à huit canons légers et de voiles carrées pour en augmenter la vitesse : on parle de  dans cette configuration de voiles. Le Renard, dernier bateau corsaire armé par Robert Surcouf, en est un exemple caractéristique.

Typologie et différences avec les gréements voisins
Le cotre est proche du sloop. Il diffère par la présence de focs multiples à l'avant (au moins deux focs pour le cotre et un seul pour le sloop).

Les voiliers à un mât sans foc ne sont pas des cotres ni des sloops, mais sont appelés  de façon générale et , , … suivant le type de voile.

Comme vu précédemment, un  est un cotre qui possède une à deux voiles carrées au-dessus de la grand-voile (hunier seul ou hunier + perroquet).

Les cotres sont généralement pontés et à quille (contrairement au dériveur).

Lorsqu'il possède un deuxième mât (tapecul) on parle de  ou de yawl, plus approprié.

Exemples de navires

Navires actuels ou encore visibles

 Le Spray est un ancien cotre américain transformé ultérieurement en yawl.
 Le Landrath Küster (1889), plus ancien hochseekutter de la région de Hambourg.
 Le Marie-Fernand (1894) est un cotre-pilote français.
 Le NAN (1896) est un des premiers plan Fife parmi les plus performants en régate de sa génération.
 Le Lady Maud (1907) est un cotre aurique anglais avec mât de flèche.
 Le Viola (1908) est un cotre écossais aurique.
 Le Tuiga (1909) est un cotre de course monégasque.
 Le Jolie Brise (1913) est un cotre de fabrication française et qui sert de navire-école britannique.
 Le Sainte-Bernadette (1926) est un cotre français à voile aurique.
 Le Nethou-Vagabond (1926) est un cotre français.
 Le Mutin (1927) est un cotre de la Marine nationale française servant de navire-école.
 Le Winibelle II (1932) est un cotre norvégien à voiles auriques construit en France.
 Le Marie Madeleine (1934) est un cotre français à tapecul, type cordier du Cotentin construit en 1934.
 L'Oiseau de Feu (1937) est un cotre français classé monument historique.
 Le Khayyam (1938-39) est un cotre à coque bois français, construit aux Pays-Bas.
 Le Vieux Copain (1940) est un cotre à tapecul, ancien thonier et monument historique depuis 1983.
 La Sinbad (1950) est un cotre bermudien français.
 La Sereine (1952) est un cotre bermudien français de .
 Le Renard est un cotre à hunier, réplique de celui du corsaire Robert Surcouf (1812).
 Le Marche-Avec (1991) cotre-sardinier de Concarneau.
 Le Saint-Michel II (1876, réplique 2011), bateau de Jules Verne et cotre de Nantes sur la base des Hirondelles de la Manche.
 Le Hope (caseyeur), cotre aurique de 1943 de Croix-de-Vie, classé monument historique depuis 1998.
 Le Saint-Quay (1947), cotre à tapecul en bois, ville de Saint-Quay-Portrieux.
 Le Skellig (2011) est une réplique de dundee langoustier d'Iroise (cotre à tapecul), construit à Douarnenez.
 La Marcelle, cotre bois à trois focs basé à Boyardville.
 Isis (1935), cotre Marconi, conçu pour la Fastnet de 1935 par Georges Baldenweck.
 Morna (1913), cotre conçu pour la Sydney-Hobart.

Navires disparus

 Le Furet au service de la duchesse de Berry.

Notes et références

Voir aussi

Bibliographie

Articles connexes
 Sloop
 Sloop-of-war
 Glossaire maritime
 Vieux gréement
 Liste alphabétique des types de bateaux

Liens externes

Type de bateau à un mât
Type de bateaux
Type de voilier
Type de gréements
Vocabulaire maritime