text:
\section{Introduction}

 The rotational velocities obtained from gas observations are one of the most
commonly used tools to study the mass distributions of spiral galaxies.  It is often assumed that the gaseous motions are purely circular
due to their low velocity dispersions.  However, the presence of a galactic bar will induce non-circular motions due to the streaming along the bar. Since bars account for two-thirds of nearby galaxies (eg. \citealt{1991rc3..book.....D, 2000AJ....119..536E, 2000ApJ...529...93K, 2002MNRAS.336.1281W, 2007ApJ...659.1176M,
2007ApJ...657..790M, 2008ASPC..396..351B, 2009A&A...495..491A, 2009ASPC..419..138M, 2010ApJ...711L..61M, 2011MNRAS.411.2026M}), it is important to properly account for these motions.

The study of the mass distribution is done by comparing the observed RC
 with the expected contributions from the gas, stars and dark matter,
assuming axisymmetry, and that the gas is in circular motions (e.g. \citealt{de-Blok:2008oq}). For the dark matter component,  an empirical or
theoretical density profile is used. There are several dark matter density profiles suggested in the literature. The two most commonly used are the
NFW profile \citep{nfw96} derived from cosmological simulations with a central cusp and the isothermal (ISO) model
(see e.g: \citealt{1985ApJ...299...59C, 1985ApJ...294..494C}) with a central flat core (see also: \citealt{1969AN....291...97E, 1995ApJ...447L..25B, 1998ApJ...502...48K}), a more general form of the dark matter density profile is also given by \cite{2001AJ....121.1952B}.
 Alternative model such as the Modified Newtonian Dynamics (MOND) \citep{Milgrom:1983lq, Milgrom:1983rr, Milgrom:1983rd} do not have a dark matter component. \cite{Milgrom:1983rr} stipulated that there is no need for a dark matter halo to explain the flatness of galaxies' rotation curves (RCs) if the law of gravity is modified below a critical acceleration a$_{0}$.
 A comparison between ISO dark matter models and MOND models, for a sample of dwarf and spiral galaxies, is given in \cite{2014MNRAS.439.2132R} but a larger sample is needed before a final conclusion can be made.

  In order to distinguish between both these and other models, RCs that represent the gravitational potential are
necessary.  RCs are often derived from observed velocity maps of gas using the tilted ring method \citep{1974ApJ...193..309R}.
This method divides the velocity map into co-centered rings and infers a variety of kinematic parameters, including the circular
velocities.  It has been implemented in  the GIPSY \citep{2011ascl.soft09018A} task {\sc rotcur} \citep{1989A&A...223...47B}.
Unfortunately, { \sc rotcur} does not correct for the non-circular motions.  There are other methods that have been developed to account
for these motions, including the publicly available DiskFit code \citep{2007ApJ...664..204S}. DiskFit creates physical models from the observed rotation velocities and extract the non-circular motions
using a $\chi^{2}$ minimization technique (for more details see : \footnote{\url{http://www.physics.rutgers.edu/~spekkens/diskfit/}}). DiskFit has proven to be able to detect weak bars \citep{2012MNRAS.427.2523K}. It was specifically designed to fit a non-axisymmetric flow pattern to
two-dimensional velocity maps \citep{2007ApJ...664..204S}. However, it is well known that the DiskFit bar flow algorithm fails when the bar is almost parallel to the major or minor axis because of the degeneracy of the velocity components \citep{2010MNRAS.404.1733S}.

 \cite{2008MNRAS.385..553D} used numerical models with pure rotation and compared the known circular velocities with the observed rotational velocities. They found that if a bar is perpendicular to the major axis of a galaxy,
the measured rotational velocities and thus the mass is over estimated and the contrary if the bar is parallel to the major axis

  We propose an alternate method to account for non-circular motions using N-body simulations.  A grid of models with different bar orientations, strengths, and bulge-disk-halo compositions is generated.
RCs from images of these models are made using {\sc rotcur}, which are then compared to the RCs calculated from the gravitational potential and its derivatives.  This comparison gives the corrections necessary for non-circular motions. To get the corrected RC for a real galaxy, the best corresponding model
from the grid of simulations is selected and the corrections derived from the simulation are applied to the actual galaxy's RC derived from {\sc rotcur}.

The paper is organised as follow:  Section \ref{data} describes the details of both the numerical simulations and the {\sc rotcur} and DiskFit algorithms.
Section \ref{res} compares the RCs derived from the simulations using {\sc rotcur} and DiskFit to the RC obtained from the
gravitational potential.  In Section \ref{case} we describe our new method of correcting RCs and use NGC 3319 as a test
case to show the importance of properly accounting for non-circular motions in mass models.  Finally, in Section 5 we present our conclusions.

\section{Data analysis}
\label{data}
\subsection{N-body simulations}
\label{sec:nbody}

We use a series of spiral galaxy simulations, with different Hubble types,
Sa, Sb, Sd, fitted to observed rotation velocities (cf \citealt{2010A&A...518A..61C}) and different radial distributions of dark matter, with either a core or a cusp
in the center, and different dark-to-visible mass ratios (maximum disk or not).
 They give a range of rotation velocities with various shapes, rising more
or less slowly with radius. We do not vary the total mass of the galaxies, since only the shapes of the rotation velocities are important, and masses can be varied by a change of units. It is acknowledged that there is a mass and size evolution along the Hubble sequence (see e.g. \citealt{2014ApJ...788...28V}), and that late-type spiral galaxies are lighter and smaller, but these can be taken into account afterwards through rescaling.
For all galaxy models, the total mass inside 35 kpc
is 2.4 10$^{11}$ M$_\odot$, with 75\% in dark matter and 25\% in baryons,
for the standard model (based on the $\Lambda$CDM cosmology) and equality between baryons and dark matter
for the maximum disk model.

\begin{table*}
\caption{Initial conditions for the various components (bulge, disk, halo, and gas) of the different models used. All models are normalized to giant galaxies to explore the different shapes. Dwarfs can be obtained through rescaling (see text).}
\label{tab:simul}
\begin{center}
\begin{tabular}{lcccccccc}
\hline
\\
Model & M$_b$ & r$_b$ & M$_d$ & r$_d$ & M$_h$ & r$_h$ & M$_{gas}$ & r$_{gas}$ \\
&10$^{10}$ M$_\odot$& kpc & 10$^{10}$ M$_\odot$  & kpc &  10$^{10}$ M$_\odot$&kpc &  10$^{10}$ M$_\odot$& kpc \\
\hline
\\
gSa & 4.6  & 2. &  6.9 & 4. &  11.5 & 10.  & 1.3  & 5. \\
gSb-st & 1.1  & 1. &  4.6 & 5. &  17.2 & 12.  & 0.9  & 6. \\
gSb-dmx & 2.2  & 1. &  9.2 & 5. &  11.4 & 12.  & 0.9  & 6. \\
gSb-nfw & 1.1  & 1. &  4.6 & 5. &  17.2 & 12.  & 0.9  & 6. \\
gSd-st & 0.  & -- &  5.7 & 6. &  17.2 & 15.  & 1.7  & 7. \\
gSd-dmx & 0.  & -- &  11.4 & 6. &  11.4 & 15.  & 1.7  & 7. \\
gSd-nfw & 0.  & -- &  5.7 & 6. &  17.2 & 15.  & 1.7  & 7. \\
\\
\hline
\end{tabular}
\end{center}
\end{table*}

 We have used two different simulation codes, in order to test
that our assumptions are not biasing the results. In both kinds
of simulations, the runs are fully self-consistent, with live dark haloes.
The first code is based on a 3D particle-mesh and the Fast-Fourier Transform  (FFT) technique to solve the Poisson equation, and the gas is represented by sticky particles (FFT-sticky particles).
  We also ran a set of simulations using the Tree-SPH code used in the Galmer project \citep{2007A&A...468...61D}.  More details on these simulations including the hydrodynamics, star formation, and feedback can be found in Appendix A. The total number of particles is 240k in the FFT-sticky code and 480k in the Tree-SPH code.

These produced different outputs for the gas particle distributions, but the effects of the bar on the observed velocity maps were the same.  Since the conclusions are the same, we will primarily examine the results for the FFT-stickly particles simulations and the results for the Tree-SPH runs can be found in Appendix B.

 For the initial conditions of the galaxies of different Hubble types,
we have followed the procedure described by \cite{2007A&A...468...61D}.
The halo and the optional bulge are modeled as a Plummer sphere,
and the stellar and gaseous disks follow a Miyamoto-Nagai density
profile.

The mass and characteristic radii of all components in
the seven initial conditions, are displayed in Table \ref{tab:simul}.
The standard model (-st) has a disk dominated by dark matter,
with a central core. A NFW model, with a cusp and a central
concentration of c = 8  has been run (-nfw), then a maximum disk model
(-dmx) with equal mass between baryons and dark matter within the optical
disk.
The initial rotational velocities, corresponding to the main variations
of the parameters, are displayed in figure \ref{fig:vrotall}.

\begin{figure*}
\centerline{
\includegraphics[angle=-90,width=15cm]{figure1.eps}}
\caption{Initial RC
s of the various models, described
in table \ref{tab:simul}. The left plot compares the various morphological types, and the right plot the various dark matter distributions.
}
\label{fig:vrotall}
\end{figure*}

The expected velocities  ($ \rm V_{expected}$) were calculated from the gravitational potential and its derivatives. More specifically, the potential derived from the disk
is averaged out azimuthally, to obtain $\Phi$(r), and the circular velocity $V_{circ}$ is

\begin{equation}
\rm V_{circ}^2 = - r \frac{d\left<\Phi\right> }{dr}
\end{equation}

\subsection{Snapshots}

The snapshots from the FFT-sticky particles simulation were extracted from the data using a projection code specifying the inclination angle and the position angle and deriving the radial velocity of the gas particles at each point of a data cube. The data cube have three axes, the first and second axis are the right ascension and declination and the third axis is the velocity in km/s. Each cubes have 50 channels with a 12.5 km/s velocity resolution.
The cube is then transformed into a fits file. The projection angle PA was varied between 10 to 180 degrees in order to cover a wide range of intrinsic bar orientations for all the snapshots.

  We select the snapshots where the bar has reached a quasi-stationary state (most of the gas have been converted into stars),
but is still strong enough, and there is enough gas remaining in the disk
to sample the rotation velocities with gas only. Indeed, the simulations do not take
into account gas accretion form the cosmic filaments, and the gas density is progressively
reduced by star formation.

\subsection{Measuring the rotational velocities}

\subsubsection{Using the tilted-ring method with {\sc rotcur}}

{\sc rotcur} uses the tilted-ring method \citep{1974ApJ...193..309R}, which divides  the observed velocity field into concentric rings and estimates the circular velocities and other kinematical parameters such as position angle (PA) and inclination using a $\chi^{2}$ minimization technique. This method assumes that the gas is moving purely along circular orbits. Each ring is characterized by the rotation center x$_{\rm c}$  and y$_{\rm c}$, the systemic
velocity V$_{\rm sys}$, the expansion velocity V$_{\rm exp}$ (assumed here to be zero), the inclination angle and PA. These parameters can be fixed or let free to vary depending on the user.
 The line of sight velocity at any position in the ring is then given by:
 \begin{equation}
\rm V(x,y) = V_{sys} + V_{C}sin(i)cos(\theta),
\end{equation}
where $\theta$ is the position angle with respect to the receding major axis measured in the plane of the sky, V$_{\rm sys}$ the systemic velocity and i the inclination angle.

$\theta$ is related to the actual PA by the following equations:
\begin{equation}
\rm cos(\theta) = \frac{- (x - x_{c})sin(PA) + (y-y_{c})cos(PA)}{R}
\end{equation}
\begin{equation}
\rm sin(\theta) = \frac{- (x - x_{c})cos(PA) + (y-y_{c})cos(PA)}{Rcos(i)}
\end{equation}

The data cubes extracted from the simulation snapshots were analyzed with the Groningen Image Processing System (GIPSY: \url{http://www.astro.rug.nl/~gipsy/}) software. The task {\sc rfits} was used to convert the fits file into a GIPSY format, then the fits headers were changed using {\sc fixhed}. The following parameters were modified in the header; the axis and the pixel size which is necessary before extracting the velocity fields. The task {\sc momnt} was used to produce the moment maps, and the rotation velocities were derived using {\sc rotcur}. The expansion velocity is fixed to zero for all the models. We choose an inclination angle of 60 degrees which is suitable for the kinematical studies. The systemic velocity ( V$_{\rm sys}$) and position angle (PA) are fixed using the following values: V$_{\rm sys}$ = 0.0 km s$^{-1}$  and PA = 0.0 degree during the fitting procedures.

The process of deriving the RCs includes three steps; firstly, the PA and inclination are held fixed using the optical values and the systemic velocity and position centre (Xpos and Ypos) are allowed to vary; secondly, the systemic velocity and the kinematic centre are held fixed and the PA and inclination are let free to vary; finally, all the above parameters are fixed and the average values are used to derive the RCs.

\subsubsection{Using the DiskFit bisymmetric model}

 DiskFit \citep{2007ApJ...664..204S} is specifically designed to correct the non-circular flows due to bars. It creates physical models from the observed velocity fields and extracts sthe velocities and other parameters from the model velocity map. DiskFit also uses a bootstrap method to estimate the uncertainty on the parameters and uses all to data during the fitting procedures.

DiskFit compares the observed velocity field with the following equation:
\begin{equation}
\begin{split}
\rm V_{model} = V_{sys} + sin(i)[V_{t}cos(\theta) - V_{2,t}cos(2\theta_{b}) cos(\theta) \\\\
\rm - V_{2,r}sin(2\theta_{b}) sin(\theta)
\end{split}
\end{equation}
where V$_{t}$ is the circular velocity, V$_{2,t}$ and V$_{2,r}$ the amplitudes of the tangential and radial component of the noncircular motions for a bisymmetric flow model.
This form of the equation is for bisymmetric flows from bars.  Moreover, DiskFit can also deal with warped galaxies.  Regardless,
if the gas is moving on purely circular orbits, this equation reduces to the key equation of the tilted-ring method.

DiskFit estimates the rotational velocities and the other parameters using a $\chi^{2}$ minimization technique:

\begin{equation}
\rm \chi^{2} = \sum^{N}_{n=1}(\frac{V_{obs}(x,y)-\sum^{k}_{k=1}\omega_{k,n}V_{k}}{\sigma_{n}})^{2}
\end{equation}
where V$_{\rm obs}$(x,y) is the observed velocity at the position (x,y) on the sky, $\sigma_{n}$ is the uncertainty, $\omega_{k,n}$ is a weighting function which includes the trigonometric factors and also defines an interpolation scheme for the projected model \citep{2010MNRAS.404.1733S}. Some of the advantages of DiskFit are listed in \cite{2010MNRAS.404.1733S}. DiskFit uses all the data in a single fit, which is necessary to detect mild distortion and also gives a better estimate of the uncertainty using a bootstrap method \citep{2007ApJ...664..204S}.
\section{Results and discussions}
\label{res}
\subsection{Results using {\sc rotcur}}

\begin{figure*}
\centerline{
\includegraphics[angle=0,width=22cm]{figure2_bw.eps}}
\caption{Three different bar positions for the model gSa (FFT-Sticky particles, T= 700 Myrs)
Top panel: the bar is perpendicular to the major axis, middle panel: intermediate position and bottom panel: parallel to the major axis.
The first column is the moment0 map, second column the moment 1 map superposed with the iso-velocity contours and the third
column the comparison between the expected velocities shown as a continuous line and the measured rotation velocities derived using {\sc rotcur} (black points). The axes of the moment maps are in pixels  (1 pixel = 5 arcsec).}
\label{stck1}
\end{figure*}

\begin{figure*}
\centerline{
\includegraphics[angle=0,width=22cm]{figure3_bw.eps}}
\caption{Three different bar positions for the model gSb (FFT-sticky particles , T = 700 Myrs see figure \ref{stck1} for details).}
\label{stck2}
\end{figure*}

\begin{figure*}
\centerline{
\includegraphics[angle=0,width=22cm]{figure4_bw.eps}}
\caption{Three different bar positions for the model gSd ( FFT-sticky particles, T = 900 Myrs see figure \ref{stck1} for details).}
\label{stck3}
\end{figure*}

\begin{figure*}
\centerline{
\includegraphics[angle=0,width=16cm]{figure5.eps}}
\caption{Standard gSb galaxy model: comparison between the expected RCs calculated from the gravitational potential as continuous lines and the average RCs for different bar orientations as filled circles with the 1-$\sigma$ error bars. The RCs of 12 simulated galaxies with different bar orientations were extracted and averaged for each snapshot (PA varies between 0 and 180 degrees with a step of 15 degrees). The epochs of the snapshots are shown on the graph.}
\label{fig:vrotstr}
\end{figure*}

 \begin{figure*}
\begin{minipage}{140mm}

  \begin{tabular}[t]{c}
         \hspace*{-6.0em} \vspace{-1.0em}
            \subfigure{\includegraphics[width=0.42\linewidth]{figure6a.eps}}\\
	   	\hspace*{-6.0em} \vspace{-1.0em}
        \subfigure{\includegraphics[width=0.42\linewidth]{figure6b.eps}}
         \hspace*{-1.0em}
        \subfigure{\includegraphics[width=0.42\linewidth]{figure6c.eps}}
        \hspace*{-1.0em} \vspace{-1.0em}
          \subfigure{\includegraphics[width=0.42\linewidth]{figure6d.eps}}\\
	   	\hspace*{-6.0em} \vspace{-1.0em}
        \subfigure{\includegraphics[width=0.42\linewidth]{figure6e.eps}}
         \hspace*{-1.em}
        \subfigure{\includegraphics[width=0.42\linewidth]{figure6f.eps}}
        	\hspace*{-1.0em} \vspace{1.0em}
	  \subfigure{\includegraphics[width=0.42\linewidth]{figure6g.eps}}
                  \end{tabular}
     \caption{This figure shows the comparison between measured and calculated RCs for all the models listed
in table \ref{tab:simul} for the snapshots with the strongest bar (the epochs are given in table \ref{tab:disp}). Lines and symbols are the same as in figure \ref{fig:vrotstr}.}
     \label{d1}
\end{minipage}
\end{figure*}

The results for the FFT-sticky particles code for three different bar orientations  are shown in figures \ref{stck1}, \ref{stck2} and \ref{stck3} for the gSa, gSb and gSd models respectively. The snapshots were taken at the following epoch T=700 Myrs for gSa, T = 700 Myrs for gSb and T = 900 Myrs for gSd. The intensity maps of the particles, which show the orientations of the bar (MOMENT0 maps) are shown in the left panels and the velocity fields with iso-velocity contours ($\Delta$V = 50 km s$^{-1}$) (MOMENT1 maps) are shown in the middle. The axes of the moment maps are in arcsec. A distance of 16.5  Mpc is adopted to convert from arcsec to parsec scale for all the models.
Comparison between the expected RCs and the measured  RCs using {\sc rotcur} are shown in the right panels. The expected RCs are presented as continuous lines and the  RCs derived using { \sc rotcur} as black circles.

  {\sc rotcur} over-estimates the rotation when the bar is perpendicular to the major axis except for the gSa model for which most of the mass comes from the bulge component. The top panels of figure \ref{stck1} shows that the measured rotation velocities using { \sc rotcur} and the expected rotation velocities are in good agreement even if the bar is perpendicular with the major axis. This is probably because the higher velocity due to the gas streaming motion along the bar is compensated by the contribution from the bulge. The differences between the measured rotation velocities and those expected from the gravitational potential are the largest when the bar is aligned with the major axis.
  Figure \ref{fig:vrotstr} shows a comparison between the expected rotation velocities from the total mass of the galaxy and the average rotation velocities (obtained using {\sc rotcur}) for four snapshots. The rotation velocities of 12 simulated galaxies with different bar orientations were extracted and averaged for each snapshot (P.A. varies between 0 and 180 in steps of 15 degrees). The errorbars are the 1-$\sigma$ standard deviations.
In the top-left panel, the bar starts to form but its effect on the derived rotation velocities is small. The two bottom panels present larger errorbars, with a maximum of 60 km s$^{-1}$ in the inner regions.

The average RCs derived from the snapshots with the strongest bars (see Table 2 for the epochs) for all the models are shown in figure \ref{d1}.  The top panel is the gSa model with an isothermal dark matter halo. The average of the measured RCs seems to be lower compared to the expected rotation velocities calculated from the gravitational potential. The errorbars are larger in the inner parts of the modeled galaxies which implies that the differences between the rotation velocities are only due to the bar orientations. These errorbars represent the variation of the derived RCs compared to the mean RCs. The gSb model (FFT-sticky) is shown in the middle panel. On the left is the model with the isothermal dark matter halo, in the middle the maximum disk model and on the right the NFW model. The gSd model is presented in the bottom panel; the standard model on the left, the maximum disk model in the middle and the NFW model on the right.

The maximum departure from the average rotation velocities (maximum standard deviation) for each model, are given in table \ref{tab:disp}. The first column is the name of the model, the second column the epoch corresponding to the strongest bar and the last column the maximum deviation from the mean velocity.

\begin{table}
\footnotesize
\caption{Maximum departure from the average velocity (i.e maximum deviation) for the snapshots with the strongest bars.}
\label{tab:disp}
\begin{center}
\begin{tabular}{lccc}
\hline

Model & Epochs & maximum deviation \\
&Myr& km s$^{-1}$ \\
\hline
\\
gSa-st & 800  & 60.72  \\
gSb-st & 1000 & 51.45  \\
gSb-dmx & 600  & 53.45 \\
gSb-nfw & 900  & 52.09 \\
gSd-st & 1000  & 57.27  \\
gSd-dmx & 700  & 68.48 \\
gSd-nfw & 900  &  25.80 \\
\hline
\end{tabular}
\end{center}
\end{table}
\subsection{Bisymmetric model results using DiskFit}

\begin{figure*}
\centerline{
\includegraphics[angle=0,width=19cm]{figure7_bw.eps}}
\caption{DiskFit results using the bisymmetric model (m=2) for the gSb model (T = 700 Myrs). Top panel: the bar is perpendicular to the major axis, middle panel: intermediate position and bottom panel: parallel to the major axis.
The first column is the moment0 map, second column the moment 1 map superposed with the iso-velocity contours and the third
column the comparison between the expected velocities shown as a continuous line and the and the DiskFit results. The mean circular velocity V$_{t}$ is shown as black circles, the tangential component of non-circular motion  V$_{2,t}$ as diamonds, radial components of the non-circular motion as squares and the expected circular velocity V$_{expected}$ as a continuous lines. $\rm \Phi_{b}$ is the bar position angle  in degrees obtained from DiskFit. The axes of the moment maps are in pixels  (1 pixel = 5 arcsec).}
\label{diskor}
\end{figure*}

\begin{figure}
\centerline{
\includegraphics[angle=0,width=9cm]{figure8.eps}}
\caption{Comparison between the projected bar position angles and those obtained from DiskFit.}
\label{barc}
\end{figure}

  An input parameter file is used to run DiskFit. This file includes the following: a fits file that contains the velocities which are used to derive the kinematics; the initial values for the position angle of the disk and bar, the systemic velocity, the axis ratio and the kinematic center. These parameters can be fixed or let free to vary. For a complete list of parameters the reader is advised to look at the original paper of \cite{2007ApJ...664..204S} and the DiskFit manual.

 The results for the gSb model (T= 700 Myrs) using the bisymmetric model is shown in figure \ref{diskor} for three different bar orientations. Top panel shows the bar perpendicular to the major axis, middle panel shows the bar in an intermediate position and on the bottom panel the bar is parallel to the major axis. The first column is the moment0 map, second column the moment 1 map superposed with the iso-velocity contours and the third column the comparison between the expected velocities shown as a continuous lines and the DiskFit results. The mean circular velocity V$_{t}$ is shown as black circles, the tangential component of non-circular motion  V$_{2,t}$ as blue diamonds, radial components of the non-circular motion V$_{2,r}$ as red squares and the expected circular velocity V$_{expected}$ as a continuous magenta lines. $\rm \Phi_{b}$ is the bar position angle  in degrees obtained from DiskFit. DiskFit is able to reproduce the expected velocities calculated from the gravitational potential and its derivatives when the bar is in intermediate positions but runs into difficulties when the position angle of the bar $\Phi_{b}$ is parallel or perpendicular to the major axis.
This shows that DiskFit produces very large values for the rotation velocities and  the errorbars when the bar is perpendicular with the major axis because of the degeneracy in the model parameters \citep{2010MNRAS.404.1733S}.

 Figure \ref{barc} compares the projected position angle of the bar $\Phi_{b, projected}$ and those obtained using DiskFit. DiskFit gives higher values as compared to the expected position angle of the bar $\Phi_{b}$ and run into difficulty when the bar is close to 90 degrees.

This is the reason why a different approach is needed when the bar is aligned with the major or minor axis. Here we propose to use N-body simulations of barred galaxies to estimate the non-circular motions.

\section{Test case : NGC 3319}
\label{case}
DiskFit and {\sc rotcur} are both very successful methods for deriving RC
s from velocity maps.  However, Section 3 uses simulations to
show that
both methods fail at recovering the true RC
 when a bar is aligned with the major or minor axis of an image.  An alternate approach may be to use simulations to correct the RCs for non-circular motions.  This will avoid many of the issues with either {\sc rotcur} or DiskFit.  We illustrate this method using NGC 3319, which has its bar aligned with the major axis, as
a test case. NGC 3319 is a gas-rich barred spiral galaxy classified as SBcd(rs) by \cite{1991rc3..book.....D} at a distance of 14.3 Mpc \citep{1999ApJ...523..540S}.   We compare the inferred mass profile for the uncorrected and corrected RCs and show that the conclusions about the dark halo structure vary greatly.  While our method still needs refinement, this result clearly demonstrates the importance
of taking into account non-circular motions.

\subsection {Observations and data reduction}
The H{\sc i} observations were obtained using the C configuration of the Very Large Array (VLA) for a total observing time of 5.75h on-source. Details of the observations are presented in \cite{1998MNRAS.294..353M}. The raw data were retrieved from the archive, edited and calibrated using the standard NRAO Astronomical Image Processing System (AIPS) packages. Data cubes were then obtained and cleaned with the AIPS task {\sc imagr} using robust0 weighting, which optimizes sensitivity and spatial resolution.
1031+561 is the phase and amplitude calibrator and 3C286 the flux calibrator. The C array data provide the proper spatial resolution for mass model analysis. The data cubes have 64 channels with 10.33 km s$^{-1}$ velocity resolution and 16 arcsecs angular resolution, which corresponds to a linear physical resolution of $\sim$1 kpc at the adopted distance of 14.3 Mpc. The moment maps were extracted from the data cubes using the AIPS task {\sc momnt}. Figure \ref{maps} shows four different maps for NGC 3319. The WISE W1 image is shown at the top left. This band is essentially free from dust extinction and gives the best representation of the stellar content of the galaxy. The moment 0 map (H{\sc i} gas distribution) is at the top right, the moment1 map (velocity field)  at the bottom left  and the moment2 map (velocity dispersion) in the bottom right panel.

The tilted ring method, implemented in the GIPSY task {\sc rotcur}, is used to derive the RC
. The moment1 velocity map was used as input for {\sc rotcur}.
The tilted ring analysis was done in three steps:
\begin{itemize}
\item First, the position angle (P.A.) and inclination angle ($i$) were fixed using the values of 37$^{\rm o}$ and 58$^{\rm o}$ found by \cite{1998MNRAS.294..353M} in order to estimate the systemic velocity and the kinematical centre. Our measured rotation centre and systemic velocity of 742 $\pm$ 2 km s$^{-1}$  are consistent with \cite{1998MNRAS.294..353M} (see their table 3).
\item Second, the systemic velocity and the rotation centre were kept fixed using the values obtained in the first step and the position angle and inclination were allowed to vary to investigate their variation as a function of radius.
\item Finally in the final step, the kinematical parameters were all fixed and only the rotation velocities were derived.
\end{itemize}
The results from the tilted ring analysis are presented in figure \ref{tilt}. The variation of the inclination as a function of radius is shown in the top panel, the position angle in the middle panel and the RCs in the bottom panel. The results from the receding half is presented as red squares, those from the approaching half as blues circles and those obtained using both halves as black diamonds.

\begin{figure*}
\centering
\begin{minipage}{140mm}
   \begin{center}
  \begin{tabular}[t]{c}

         \hspace*{.0em} \vspace{.0em}
           \subfigure{\includegraphics[width=0.54\linewidth]{figure9a.eps}}
	   	\hspace*{1.50em} \vspace{.0em}
        \subfigure{\includegraphics[width=0.54\linewidth]{figure9b_bw.eps}} \\
         \hspace*{.0em}
        \subfigure{\includegraphics[width=0.55\linewidth]{figure9c_bw.eps}}
        \hspace*{.0em} \vspace{.0em}
          \subfigure{\includegraphics[width=0.55\linewidth]{figure9d_bw.eps}}\\
	   	\hspace*{.0em} \vspace{0.0em}
                       \end{tabular}
     \caption{This figure shows several maps of NGC 3319. The top left panel shows the WISE W1 band (3.4 microns) image, where the bar and spiral arms are clearly seen; the moment0 map (H{\sc i} distribution) is shown in the top right panel, the moment1 map (H{\sc i}  velocity field)
in the bottom left panel and the moment2 map (H{\sc i} velocity dispersion) in the bottom right corner. }
     \label{maps}
  \end{center}
\end{minipage}
\end{figure*}

\begin{figure}
\centerline{
\includegraphics[angle=0,width=10cm]{figure10.eps}}
\caption{Tilted ring model results obtained with the GIPSY task {\sc rotcur}. The variation of the inclination as a function of radius is shown in the top panel and the position angle (PA) variation in the middle panel. The RC presented in the bottom panel was obtained with all the kinematical parameters, including PA and the inclination, kept fixed to their average values.
 The results from the receding side are presented as red squares, those from the approaching side as blue circles and from both sides as black diamonds. The lines correspond to PA= 37$^{\rm o}$ and i = 58$^{\rm o}$.}
\label{tilt}
\end{figure}

\subsection {Model-based correction to the RC}
\label{corr}
As discussed in section \ref{res}, the RC is under-estimated when the bar is aligned with the major axis because of the gas streaming along the bar.
Therefore, the effect of those non-circular motions need to be estimated, and a correction needs to be applied to the RC before it can be used for the mass models.

 We introduce the following step to correct the RCs for the non-circular motion induced by the bar:
\begin{itemize}
  \item The correction is derived from the differences between the expected RC of the model, which is calculated from the true gravitational potential of the modeled galaxy, and the observed RC measured using the tilted ring method ({\sc rotcur})
  \item The correction is scaled in terms of velocity using the $V_{max}$ ratio, i.e. ($\frac{V_{max, object}}{V_{max, model}}$) and in terms of radius using the ratio between the disk scale lengths, i.e. ($\frac{R_{d, object}}{R_{d, model}}$)  before being used to correct the RC of an actual galaxy.
  \item The modeled galaxy (model) and the actual galaxy (object) should have similar bar properties, the distance also have to be taken into account.
\end{itemize}
The correction is done using the following
\begin{equation}
V_{corrected} = V_{uncorrected} + correction\times\frac{V_{max, object}}{V_{max, model}}
\end{equation}
where $ \rm correction=V_{obs, model} - V_{expected}$, V$_{obs, model}$ is the observed velocities obtain from {\sc rotcur}, V$_{expected}$ the expected circular velocites; V$_{corrected}$ and V$_{uncorrected}$ are the corrected and uncorrected rotation velocities of NGC 3319 respectively.
\\

 To apply the corrections, the data from the model were normalized by the optical scale length in radius and by the maximum velocity in velocities using the steps described above. The data is then extrapolated to obtain the correction at a given radius. The distance of NGC 3319 is used to convert from angular scale into physical scale.
Comparison between the corrected and uncorrected RC is shown in figure \ref{rcs}.

Despite the fact that NGC 3319 is classified as a SBcd galaxy, the gSb model presented at the bottom panel of figure \ref{stck2} is used to derive the corrections. This is because the gSd model does not have a bulge component (see table \ref{tab:simul}) and that the bulge-to-disk (B/D) ratio of the gSb model obtained from the ratio between the bulge mass and disk mass given in table \ref{tab:simul} M$_{b}$/M$_{d}$ = 0.239 is very similar to the B/D = 0.24 of NGC 3319 estimated from the 3.6 micron surface brightness profile.

In this illustrated test case, we do not pretend to accurately correct for the non-circular motions induced by the bar. In the continuation of this work, we intend to match even more accurately the simulated galaxies to the actual galaxies. However, we think that the gSb simulation used is close enough to NGC 3319 to show clearly how not taking into account the effect of bars can lead to deriving very different parameters for the derived dark matter component.
We still have to investigate if it is the best way to scale the model to the actual galaxies. However, this is surely close enough to serve the purpose of this study.

\begin{figure}
\centerline{
\includegraphics[angle=0,width=9cm]{figure11.eps}}
\caption{Comparison between the model-corrected and uncorrected RCs.}
\label{rcs}
\end{figure}

\subsection {Mass model}
\subsubsection{Dark Matter Halo component}
The distribution of DM is characterized by a density profile. The observationally motivated pseudo-isothermal halo (ISO) and the cosmologically motivated Navarro, Frenk and White (NFW) \citep{nfw96} profiles are widely used.
The mass model is done by comparing the observed RCs with the quadratic sum of the luminous and dark matter components using a chi-squared minimization technique.  The mass models were carried out using the GIPSY tasks {\sc rotmas} and {\sc rotmod}.

The RC is given by:
\begin{equation}
\rm V_{rot}^{2} = V_{gas}^{2} + V_{*}^{2} + V_{halo}^{2}
\end{equation}
where $V_{gas}$ is the gas contribution, $ V_{*} $ the stars contribution and $V_{halo}$ the contribution of the dark matter component.

\subsubsection*{The pseudo-Isothermal (ISO) Dark Matter (DM) Halo Model}

The pseudo-isothermal (ISO) dark matter halo is a  core-dominated type of halo. The ISO density profile is given by
\begin{equation}
\rm \rho_{ISO}(R)={\rho_0 \over 1+({R\over R_c})^2}
\label{eq:ro_iso}
\end{equation}
where $\rho_0$ is the central density and $R_c$  the core radius of  the halo. The velocity  contribution of a ISO halo is given by:
\begin{equation}
\rm V_{ISO}(R)=\sqrt{4\pi~ G~\rho_0~ R_c^2(1-{R\over R_c}~ atan ({R\over R_c}))}
\label{eq:v_iso}
\end{equation}

We can describe the steepness of the inner slope of the mass density profile with a power law $\rho \sim r^\alpha$.
In the case of the ISO halo, where the inner density is an almost constant density core, $\alpha = 0$.

\subsubsection*{The NFW DM Halo Model}

The NFW DM halo profile was derived from cosmological simulations and it is commonly accepted in the $\Lambda$CDM framework. The NFW halo density  profile is described by:

\begin{equation}
\rm \rho_{NFW}(R)={\rho_i \over {R\over R_S} (1+{R\over R_S})^2}
\label{eq:ro_nfw}
\end{equation}
where $\rho_{i} \approx 3H_{0}^{2}/(8 \pi G)$ is the critical density for closure of
the universe and $R_{S}$ is a scale radius. The  velocity contribution corresponding to this halo  is given by:
\begin{equation}
\rm V_{NFW}(R)=V_{200}~\sqrt{{ln(1+cx)-cx/(1+cx) \over x(ln(1+c) -c/(1+c))]}}
\label{eq:v_nfw}
\end{equation}
 where $\rm V_{200}$ is  the velocity at the virial radius $\rm R_{200}$,
  $\rm c = R_{200}/R_S$ gives the concentration parameter of the halo and  x is defined as $\rm R/R_S$. The relation between $\rm V_{200}$ and $\rm R_{200}$ is given by:

  \begin{equation}
\rm V_{200}= {R_{200} \times H_0 \over 100}
\label{eq:v200}
\end{equation}
where $\rm H_{0}$ is the Hubble constant taken as  $\rm H_{0}=72.0 \ km \ s^{-1} \  Mpc^{-1}$ \citep{2009ApJS..180..225H}.

\subsubsection{Luminous matter Components}

\subsubsection*{Gas Contribution}

The contribution from the gas is estimated from the moment0 maps. The task {\sc ellint} is used to compute the H{\sc i} gas density profile  using the kinematic parameters obtained with {\sc rotcur}. {\sc ellint} divides the moment0 map into concentrated rings and estimates the density for each ring.
The output from {\sc ellint} is then used in  {\sc rotmod} to calculate the gas contribution in the mass model, assuming an infinitely thin disk.
The profile was multiplied by 4/3 to take into account the primordial Helium contribution.

\subsubsection*{Stellar Contribution}
\label{sec:stellar}

The SPITZER 3.6 microns surface brightness profile is used to calculate the stellar contribution. Near-Infrared probes most of the emission from the old stellar disk population. It is also less affected by dust and therefore represents the bulk of the stellar mass.  The data were retrieved from the SPITZER archive. After  the foreground stars were removed, the images were fitted with concentric ellipses using the {\sc ellint} task in GIPSY. The results were then converted into a surface brightness profile in mag/arcsec$^{2}$ using the method in \cite{2008AJ....136.2761O}.

The surface brightness profile is corrected for inclination and galactic extinction before being converted into mass density.
 The method used by \cite{2008AJ....136.2761O} was also adopted to convert the luminosity profile into a mass density profile.
 The density profile is given by:
\begin{equation}
\rm \Sigma[M_{\odot} pc^{-2}] = \Upsilon^{3.6}_{*} \times 10^{-0.4 \times (\mu_{3.6} - C^{3.6})}
\end{equation}
where  $\Upsilon^{3.6}_{*}$ is the stellar mass-to-light ratio in the 3.6 microns band, $\mu_{3.6}$ the surface brightness profile and C$^{3.6}$ is a constant used for the conversion from mag/arcsec$^{2}$ to L$_{\odot}$/pc$^{2}$.
C$^{3.6}$ is given by:

\begin{equation}
\rm C^{3.6} = M_{\odot}^{3.6} + 21.56
\end{equation}
where M$_{\odot}^{3.6}$ is the absolute magnitude of the Sun in the 3.6 microns band.
Using the distance modulus formula and the distance to the Sun, \cite{2008AJ....136.2761O} found:
\begin{equation}
\rm M_{\odot}^{3.6} = m_{\odot}^{3.6} + 31.53 = 3.24
\end{equation}

 \subsubsection*{The bulge-disk decomposition}

 The surface brightness profile in figure \ref{bulge} clearly shows that this galaxy has a bulge in the center, thus a bulge-disk decomposition is needed to better constraint the contribution from the stellar component.

 \begin{figure}
\centerline{
\includegraphics[angle=0,width=9cm]{figure12.eps}}
\caption{Bulge-disk decomposition, the green line is the best fit for the disk, the blue for the bulge and the dashed magenta line the sum of the contribution from both components.}
\label{bulge}
\end{figure}

The disk component was fitted with an exponential disk using the following equation

\begin{equation}
\mu (r) = \mu_{0} + 1.10857\frac{R}{R_{d}},
\end{equation}

where R$_{d}$ is the disk scale length and $\mu_{0}$ the central surface brightness. The remaining profile is fitted with a Sersic profile by letting the Sersic index n, the effective radius R$_{e}$ and the effective surface brightness $\mu_{e}$ as free parameters.
The bulge is therefore described by

\begin{equation}
\mu (r) = \mu_{e} + 2.5b_{n}[(\frac{R}{R_{e}})^{1/n} + 1],
\end{equation}
where b$_{n}$ = 1.9992n - 0.3271 for 0.5 < n < 10 \citep{1989woga.conf..208C}
The best fit result shown in figure \ref{bulge} gives R$_{d}$ = 5.77 $\pm$ 0.06 kpc, $\mu_{0}$ = 18.66 $\pm$ 0.02 mag for the disk and n = 0.87 $\pm$ 0.02, R$_{e}$ = 2.04 $\pm$ 0.05 kpc and $\mu_{e}$ = 21.74 $\pm$ 0.31 mag for the bulge.

 \subsubsection*{Mass-to-light ratio}

 The mass-to-light ratio ($\Upsilon_{*}$) for the IRAC1 band is normally derived using the J-K color (see \citealt{2008AJ....136.2761O}, \citealt{de-Blok:2008oq}). However, this method gives a higher  mass-to-light ratio for the disk component than the bulge component which is unphysical. \cite{2013ApJ...773..173D} uses chemo-spectrophotometric galactic evolution (CSPE) models to constrain the mass-to-light ratio of nearby galaxies as function of radius. We use their results to estimate the mass-to-light of NGC 3319.  NGC 3319 and NGC 2403 have the same morphological type (SBcd) and similar maximum velocity but NGC 3319 has a larger bulge compared to NGC 2403. The values used for the mass model are given in table \ref{mas}.

\subsection{Results}
The mass model results for the uncorrected and corrected RC
s are presented in figure  \ref{nfw} for the ISO and NFW models. The observed RC is shown as filled black circles with error bars, the gas contribution as dashed green lines, the stellar disk contribution as dashed red lines, the stellar bulge contribution as long-dashed blue lines and the contribution from the dark matter halos as dashed magenta lines. The continuous lines are the best-fit models to the RC. Table \ref{mas} summarizes the results for the ISO and NFW models. The columns are described as follows, the first column is the type of DM halo used, the second column gives the parameters of the fits, the third and fourth columns are the results.
For the ISO models, the dark matter halo is much more centrally concentrated when the corrected RC
 is used with a R$_{C}$ $\sim 1$ kpc compared to $\sim 5$ kpc for  the uncorrected RC
 and  a much larger $\rho_{0}$ (see table \ref{mas} for details). It is clear that the corrected and uncorrected RC give very different results for the dark matter parameters which shows the importance of those corrections for non-circular motions. The same is true for
the NFW models where the concentration index c is five times larger when the corrected RC is used and R$_{200}$ much smaller. Both the ISO and NFW models gives very good fits to the corrected RC with smaller $\chi^{2}_{r}$. This confirms that the parameters of the dark matter halo are strongly affected by the non-circular motions induced by the bar, especially when the bar is aligned with the major axis. A large portion of the mass will be missed if the RC
 is not corrected and different conclusions could be drawn from the dark matter parameters.
The difference between the uncorrected and corrected RC is still significant even after the bulge component has been taken into account. This is a clear demonstration that corrections must be applied to the observed RC so that it really represents the dynamical mass of barred systems.

\begin{table}
\caption{Results for the ISO and NFW dark matter halo models using the uncorrected and corrected RCs.}
\begin{center}
\begin{tabular}{c c  c  c }
\hline
\\
Halo Model&Params &Uncorrected RC&Corrected RC\\
\hline
ISO& $\rho_{0}$& 5.55$\pm$0.99 & 74.08$\pm$15.15\\
 & R$_{c}$& 6.91$\pm$1.11&1.34$\pm$0.16\\
 &$\Upsilon_{d}$& 0.25&0.25 \\
&$\Upsilon_{b}$& 0.40&0.40 \\
&$\chi^{2}_{r}$&1.35&0.75\\\\
NFW& c& 0.43$\pm$0.01&5.18$\pm$0.73\\
 & R$_{200}$&  147.25$\pm$11.00&56.46$\pm$3.44\\
 &$\Upsilon_{d}$&0.25 &0.25 \\
&$\Upsilon_{b}$&0.40&0.40 \\
&$\chi^{2}_{r}$&3.24&1.44\\

\hline

\end{tabular}

\addtocounter{footnote}{-2}
\end{center}
\footnotesize{{\it Notes}:  $\Upsilon_{d}$ is the mass-to-light ratio for the stellar disk and $\Upsilon_{b}$ for the bulge. The central DM density $\rho_{0}$ is given in units of 10$^{-3}$ M$_{\odot}$ pc$^{-3}$; R$_{c}$ and R$_{200}$ are in kpc.}\\

\label{mas}
\end{table}

\begin{figure*}
\centerline{
\includegraphics[angle=0,width=18cm]{figure13.eps}}
\caption{Mass models using ISO DM halo model (top) and NFW DM halo model (bottom) for the uncorrected (left) and model-corrected (right) RCs. Lines and symbols are shown on the top left corner of the first panel.}
\label{nfw}
\end{figure*}

\section{Summary}
\label{disc}

We have presented the analysis of snapshot observations of N-body/hydrodynamic simulations of barred spiral galaxies with different bar strengths and orientations to quantify the non-circular motions induced by a bar. .
In the simulations, the bar forms naturally due to gravitational instabilities. Therefore, snapshots of simulated galaxies spanning a wide range of bar strengths and bar orientations can be extracted and analyzed.
Several models with different morphological types and dark matter halo distributions are analysed.

The results from the tilted ring method using {\sc rotcur} show that the rotational velocities are largely under-estimated if the bar is parallel to the major axis and over-estimated if the bar is perpendicular except for an Sa galaxy which has an important central bulge for both simulations. This is consistent with \cite{2008MNRAS.385..553D}. This corresponds to the elongated orbits of the gas along the bar, which enhance the velocities at pericenter and reduce them at apocenter. Part of the gas and dust are moving alongside the bar which increases the measured circular velocity when the bar is parallel to the major axis and decreases it if the bar is aligned with the minor axis. The effect is smaller when the bar is in an intermediate position.

We also use DiskFit for our analysis. DiskFit is specifically designed to fit non-axisymmetric distortions from 2D velocity maps \citep{2007ApJ...664..204S}.
However, DiskFit works only when the bar is not aligned with the symmetry axes of the projected galaxy, and strong distortions are seen in the velocity field.

\cite{2010MNRAS.404.1733S} noted that the circular velocity is biased low when the bar is parallel to the major axis (apocentre) since the gas follows an elliptical pattern and that the circular speed should be higher when the bar is aligned with the minor axis.

The test case in section \ref{case} shows that the distribution of mass in NGC 3319 is very affected by the non-circular motions induced by the bar. For example, the central dark matter core is much more compact when the corrected RC is used. The ISO and NFW results are very different in all cases for the corrected and uncorrected RCs.

For future work, snapshot observations with different bar strengths and orientations will be studied to estimate the corrections that need to be applied to  the observed rotation velocities of a sample of barred galaxies with a variety of bar strength and bar orientation. A sample of barred galaxies with different bar sizes and orientations will be selected and modeled. This will help us to compare the results from the observations and the simulations for the individual galaxies.The main aim of this future work is to try to match as closely as possible the parameters of the model and the parameters of the galaxies, especially those of the bar. In particular, we will try to closely match the DM halo-to-luminous disk ratios.

\section*{Acknowledgments}
We thank the anonymous referees for the comments and suggestions. CC's work is based upon research supported by the South African Research Chairs Initiative (SARChI) of the Department of Science and Technology (DST), the SKA SA and the National Research Foundation (NRF); ND and TR's work are supported by a SARChI's South African SKA Fellowship. We thank T. Jarrett for the Wise image.


text:
The Johannes Kepler ATV, or Automated Transfer Vehicle 002 (ATV-002'''), was an uncrewed cargo spacecraft built to resupply the International Space Station (ISS). It was launched on February 16, 2011 by the European Space Agency (ESA). Johannes Kepler carried propellant, air and dry cargo weighing over , and had a total mass of over , making it, at the time, the heaviest payload launched by the ESA. The spacecraft was named after the 17th-century German astronomer Johannes Kepler.Johannes Kepler was the second ATV cargo resupply vehicle to be launched, following the Jules Verne mission of 2008. Johannes Kepler carried around five tons more cargo than Russia's Progress-M resupply spacecraft, and about 1.5 tons more than the Japanese HTV. The ATV used  of fuel to boost the ISS's altitude from 350 to 400 km.

Many of the supplies aboard the ATV were used for the Space Shuttle mission STS-133 and the ISS Expedition 26. A Reentry Breakup Recorder was placed aboard the ATV before it undocked from the ISS on June 20,2011. Johannes Kepler performed a destructive re-entry as intended on 21 June 2011, with its remains impacting the Pacific Ocean.

SpacecraftJohannes Kepler consisted of two sections: the Propulsion Module, with four main engines and 28 smaller maneuvering thrusters, and the Integrated Cargo Carrier, which attached directly to the ISS and could hold up to eight standard payload racks. The four solar wings of the spacecraft provided up to 4,800 watts of electrical power to its rechargeable batteries.

The ATV's rendezvous and docking system mounted a telegoniometer, which functioned as a radar system, and two videometers, which fired laser pulses at cube-shaped reflectors on the ISS' Zvezda service module for range detection. The nose of the spacecraft contained rendezvous sensors and Russian docking equipment.

Specifications

Mission payload

 Source: NASAGeoFlow IIJohannes Kepler delivered the GeoFlow II hydrodynamics experiment container to the ISS. This experiment was designed to observe liquid movements in microgravity, and compare them with computer simulations, thus helping scientists to understand convection currents within the Earth's mantle.

Mission summary

Launch
[[File:ATV-2 launch from ISS.jpg|thumb|right|Johannes Keplers launch as seen from the ISS. The ATV is the thin white plume rising from the Earth in the center of the image.]]
On 16 February 2011 UTC, Johannes Kepler was launched on an Ariane 5ES rocket from the Guiana Space Centre in Kourou, French Guiana. The launch was conducted by Arianespace on behalf of the ESA.

The first launch attempt, on 15 February 2011, was halted four minutes before lift-off, due to an erroneous signal from one of the rocket's fuel tanks.

Docking

Docking with the ISS was completed on 24 February 2011 at 15:59 UTC, after a 15-minute delay. The spacecraft traveled over eight days to catch up with the space station, and arrived at the aft port of the station's Zvezda service module. During the rendezvous operations, ATV-2 traveled a total of 2.5 million miles. The docking occurred as ATV-2 and the ISS flew over the coast of Liberia in western Africa. Hooks and latches engaged a few minutes later to firmly attach ATV-2 to the ISS.

The Johannes Kepler mission marked the first time European astronauts were on board the International Space Station during an ATV mission, with Italian astronaut Paolo Nespoli welcoming the ATV's arrival. ESA astronaut Roberto Vittori was also aboard the ISS at the same time as the ATV, having arrived on Space Shuttle Endeavour on the STS-134 mission in May 2011.

ISS altitude IncreaseJohannes Kepler was used to boost the ISS's standard altitude from about 350 kilometers (220 statute miles) to 400 km (248 miles). The higher altitude has lower atmospheric drag, which reduces the propellant needed annually to maintain the station's altitude from 6,800 kg (15,000 lb) to roughly 3,630 kg (8,000 lb), depending on atmospheric conditions. The ATV used about 4,500 kg (9,900 lb) of rocket fuel to accomplish this change, with the reboost occurring incrementally over several months.

End of mission and deorbit
On 20 June 2011, Johannes Kepler'' undocked from the ISS. At 18:30 UTC (20:30 CEST) that same day, while preparing to deorbit, the ATV was forced to conduct a debris-avoidance maneuver, using some of its remaining fuel to move into a safe orbit after NASA warned of a potential collision with orbital debris. On 21 June 2011, the ATV deorbited, burning up in the atmosphere as planned over the South Pacific Ocean at around 22:44 CET.

ATV missions

See also

H-II Transfer Vehicle
Progress spacecraft
Uncrewed spaceflights to the International Space Station

References

External links

ESA – ATV
ESA – ATV blog
Mission Overview Video
Launch Kit Flight 200 Ariane 5ES ATV Johannes Kepler

Automated Transfer Vehicles
Johannes Kepler
Spacecraft launched in 2011
Spacecraft which reentered in 2011
Supply vehicles for the International Space Station

redpajama_set_name: RedPajamaWikipedia


Summer is almost here so I chose what I would wear to Galveston beach in May or June. I chose a dress swimsuit for my figure, topped it with a floppy hat,sunglasses,wedges,beach tote and a cute little flower bracelet. I love this combo and I know I will be looking fly with my husband and kids.
Hi heel lovers my daughter and I finally got around to revamping her heels and I tell you it was fun for our first project. We had already shopped for some gems and chain to decorate the heels, we just used a hot glue gun to glue everything in place. Hot glue can get a little sticky and stringy and we did burn ourselves at least once lol! nothing major though.
I think we did pretty good on those Lacey little things, we probably could have did more to the heel but we just worked with what we had. There may have been more we could have done , like cut off all the lace and made a glittery heel or painted the heel. There are so many possibilities to making over heels so the next time we'll see what we can come up with. Anyway thank for reading my post and please tell me what you think.


Posted by SkandhusMommy on 11/10/09 • Categorized as Me..me..me..
what a nice! bath is playtime to rai!
Today my baby was born! Frank Luis Gomez became part of our family at 9:23 AM!Before the baby it was intimidating, but after reading a few books, it was no longer a worry of mine.


The Detroit Red Wings have a chance to regain the Western Conference lead Tuesday night, but they need start tightening up defensively after another abysmal effort in their last game.
The woeful Phoenix Coyotes, surprisingly, could create more problems in the Wings' end of the ice.
Detroit (43-15-8) hopes to move atop the West and bounce back from a blowout home loss in its last game when it hosts the Coyotes.
The Red Wings have 94 points and are tied with San Jose, which plays at Minnesota later Tuesday night. The focus for Detroit, though, may be less on its current position in the standings and more on rebounding from their second lopsided defeat in four games.
The Wings fell 8-2 to Columbus on Saturday night, as Chris Osgood gave up seven goals on 23 shots before being pulled in the third period for Ty Conklin. Detroit was outshot 46-23 and outscored 4-1 in the third period.
"You don't want to play like this, especially in front of your home fans," center Henrik Zetterberg said. "Today, it was breakaways we gave them. You have to execute, make the passes. We have to step up and play better as a group."
The alarming performance came one week after an 8-0 rout at Nashville, when Conklin gave up four goals in the first 9:51 on Feb. 28 before giving way to Osgood, who yielded another four on 14 shots.
Sloppy play and turnovers in their own zone cost the Red Wings in both blowouts, which were sandwiched around a pair of wins.
"We didn't give ourselves a chance. We hung our goalie out to dry - both of them," coach Mike Babcock said after Saturday's defeat. "We got out of sync by turning the puck over early and we never really got it going."
Osgood has won five straight against Phoenix, although he's given up 17 goals in his last five games - a stretch that includes a shutout of St. Louis last Tuesday. Conklin is 7-1-0 with a 2.42 goals-against average in his previous nine appearances, but allowed five goals in his only career start against the Coyotes - a 6-3 road loss Jan. 20.
The Red Wings could get an offensive boost Tuesday from the expected return of right wing Tomas Holmstrom from hernia surgery. Holmstrom, who hasn't played since Jan. 29, has seven goals and nine assists in his last 15 games against Phoenix.
The Coyotes (28-33-5) have been dominated by the Wings recently, going 1-9-1 in the last 11 meetings. Phoenix, however, has scored 14 goals in the last three matchups, earning the Jan. 20 win and picking up a point in a 5-4 shootout loss at home Dec. 13.
The Wings took the most recent meeting 5-4 on Feb. 4 at Joe Louis Arena on Nicklas Lidstrom's goal with 39 seconds left.
Phoenix's Ed Jovanovski and Joakim Lindstrom each have two goals and three assists in the last three matchups with Detroit, while teammate Enver Lisin has two goals over that span.
While Phoenix has managed to generate offense versus Detroit, the Coyotes haven't done much of that against anyone else lately. They've averaged 2.1 goals in dropping 14 of 18 and have totaled eight goals while going 1-5-0 in their last six.
In Sunday's 3-2 road loss to the New York Islanders, they failed to convert on seven power-play opportunities, including a pair of two-man advantages.
"We didn't capitalize on either five-on-three," coach Wayne Gretzky said. "I believe you should score on every five-on-three situation."
Phoenix has been outscored 49-28 in its last 11 games against Detroit. The Red Wings have won five straight over the Coyotes at Joe Louis.


The little girl knows just what needs to be done to get ready for Christmas — choose a tree, back cookies, decorate the house — but Biscuit is so excited he can't seem to sit still.
Scratch and sniff the scents to find out what that silly puppy has his nose in now!
This entry was written by saurabh, posted on November 15, 2007 at 3:36 am, filed under Baby-3 and tagged All 4-for-3 Deals, Alyssa Satin Capucilli, Animals, Baby-3, Basic Concepts, Biscuit, Book Characters, Christmas, Dogs, Fiction, HarperFestival, Holidays & Festivals, People & Places, Popular Characters, Sense & Sensation, Stores. Bookmark the permalink. Follow any comments here with the RSS feed for this post. Both comments and trackbacks are currently closed.


"I want to thank Sherrie and all of Models Inc. for all of my success in my career. Thank you."
"I have worked with Sherrie for a few years, with different companies and on many projects.
- Sarah Franko, Technical Designer at Gymboree, Inc.
We switched agencies a couple years ago to Models Inc so that we could have our whole family handled by the same agency. I had talked to an on set teacher at a shoot one day who spoke very highly of Sherrie for representing kids and families. I wasn't sure if she would also be a good fit for my husband and I since we did a lot of industrials and corporate jobs but after meeting Sherrie we were totally won over by her sincerity and professionalism. We switched over the whole family and have never regretted it for a minute. We continue to be pleased with the type of work that Sherrie secures for us and would recommend her to any actor or model regardless of their age. Her, as well as her staff are always friendly and happy to answer any questions we have or accommodate our schedules which having experienced other agents is definitely not always the case.
It is always a pleasure to work with Sherrie. She is fast, reliable and always there when you need her. We have been saved by her many times during last minute changes and cast calls. Would love to keep this great business relationship with her!
Thank you very much Sherrie and Model's Inc.!
My daughter and I have been with Model's Inc for several years now and have had amazing opportunities both as individuals as well as together on set cast as a 'real-life' mom and daughter pair. From interacting with Monitor lizards longer than I am tall, to yoga postures and getting to soar down the steep streets of San Francisco by bicycle, sums up just a few of our wonderful experiences made possible by Sherrie and team at Model's Inc.
I was always under the assumption that the work was very limited in the local area but have been pleasantly surprised at all of the opportunities provided by Model's Inc., not to mention the vast variety in the type of work available as well and the overall professionalism throughout.
We've really enjoyed all of the connections we've made over the years and have been able to constantly challenge ourselves allowing us to grow and flourish both personally and professionally. We truly appreciate all of work to date, the solid portfolio we've been able to establish and look forward to many more opportunities to come!
I could not imagine where I would be in my life right now without Sherrie and Models Inc.The things that I've learned, adventures I've experienced and the great memories and friendships that I've built in this first year, I owe all to Sherrie. Through out the beginning of this journey I've always felt comfortable, safe, and professional. Whenever I had a question or needed advice, Sherrie was always there for me. Models Inc. took a chance on me, to represent me, and to guide me in my path and for that I am forever grateful.This is just the beginning and I can't wait to see what the future has in store for us!
We have been working with Sherrie & Models Inc. for many years and it's always easy. Models Inc. is our "Go To" talent agency with a large and diverse client base, they seem to have the perfect fit for any production. The actors we've hired over the years have always been pleasant and professional, and when we plan a shoot with Sherrie, talent is the last thing we have to worry about. We highly recommend Sherrie and Models Inc.
I started with Models Inc. when my daughter was 12 months old. Having researched a handful of agencies in S.F and after speaking with their agents, it was evident that Models Inc. was the place for us. Sherrie is not only professional and highly respected in the industry but friendly and approachable. Fast forward 6 years, I now have 3 kids who all are signed with Models Inc., not to mention myself and my husband! Sherrie has successfully submitted my entire family for jobs that we have gotten to shoot together. It has become somewhat of a hobby in our house hold. If you are new to the industry, don't make the mistake of thinking you need an agent in the city. Our very own Sherrie Garcia of Models Inc. here in Walnut Creek is the real deal, equal if not better than the ones whose names you here thrown around.
Sherrie and Models Inc. are always quick to respond, will work after hours to help a project, provide quick service and billing, and have an amazing follow through with talent. They are always eager to work on any project possible and it is always a pleasant, stress-free experience working with them. They are my go-to agency!


Did you get it working?
It may not be the same issue, but on a friend and family members computers all I did was install and run JarFix and then try the optifine install again.
Step 4 wont work for me It just says The system cannot find the file C:\ProgramData\Oracle\Java\javapath\java.exe. ????
Alright. heres what happened to me and i solved it. My problem=Opens up and closed in a blink of da eye.
4. cont. the cmd and now press [enter]. Bam it runs.
If you are trying to run optifines' auto installer and are still having trouble with changing the file it opens with. Open a command prompt, write "java -jar "(needs the space after -jar) then drag and drop the jar onto the command prompt before hitting enter. This should run with the most recently installed version of java.
Benefits of being a programmer You know some of these other ways around problems.
Well if your Minecraft runs at 4-8 fps I'd recommend not to use Optifine. It will make your game even slower, due to it being more for the computer to handle. And all the mod does is to make the graphic settings more customizable. But if you don't know how to do it already you shouldn't use OF.
GUI Scale: doesn't really matter, try smaller if it still lags.
Entity shadows, Alternate blocks and View bobbing doesn't really matter either, try to turn them off if it still lags.
It has happened to forge!!!! What do we do?!
Have you tried deleting system32?
Besides, in newer versions System32 is a protected folder.
Easy tip for everyone in future, if having .jar files, keep them with Java. For .zip, .rar or .7z, use 7-zip or WinRAR.
Well, not all Windows Computers. Mine did. But if it doesn't, it is best to assign them to Java.
Where Optifine.jar is whatever the Optifine JAR file's name is. Save it as install.bat, put it in the same place as the Optifine JAR, and run it.
I did this second way and my computer says "a java exception has occured."when i try to open the file.Please help if you can.
I have the same problem. When i try to open the javaw.exe file nothing happends for some silly reason.
2) move it somewhere easy to access, like your desktop.
IF it still does not show up after that step, go to choose a default program again, but instead scroll down to where it says 'Look for another program(or app on win 8) on this PC'. Then navigate to C:\Program Files (x86)\Java\JAVA VERSION HERE\jre\bin\java.exe. Select that program and you should now be able to run the optifine installer.
4) If you have not already selected Java to run the optifine installer, do so now. A popup should appear saying install Optifine (Version) for minecraft.
6) A popup will appear saying that optifine has installed. This does only take a split second, so do not be worried that it was fast.
Right-click it and go to "Open with..." and select the Java runtime. If it gives you the choice, make that the default for JAR files.
And why did you uninstall WinRAR?


I am indeed very much pleased to note your keen interest in joining the Noor Majid Ayurvedic College. As a Principal of the College, I cordially welcome you all. I must say that your critical wisdom is reflected in selection of our college and the courses for your further studies.Observing young people like you all around me, sensing their hopes, aspirations, ambitions and vision, I must say that future of young generation is full of opportunities and promises. At our College, we offer a Congenial Atmosphere; that include modern facilities of computers and good laboratories, rich libraries, study rooms, OPD etc.
Our faculties are motivated and are student centric. They help students to meet their goals and objectives by imparting quality education and trainings. 'Quality education at affordable costs' is our mission. Our qualified, young, energetic and enthusiastic teaching staffs are always on forefront to assist the students. It helps in overall development of the students for facing the competition and challenges of the knowledge era.
You will be happy to know that the track record of achievements of our colleges is indeed commendable. Required facilities at colleges are constantly upgraded. Learning and extra-curricular activities enable our students to bring laurels in Professionalism. At this juncture, I appeal you to commit to your resolution. I want you to really work on it hard and with sincerity. We are with you to help. I wish you all the best for your career.


text:
Import stylesheets using `@import` and an optional media query. Pass a string or
an array of paths to the `path` option in where to search for stylesheets.
Handle recursive & relative imports.

## Install

```bash
$ npm install --save rework-import
```

## Usage

As a Rework plugin:

```js
var imprt = require('rework-import');

rework(data)
    .use(imprt())
    .toString();
```

Example with all options

```js
// using multiples paths
rework(data)
    .use(imprt({
        path: [
            'path/to/your/stylesheets',
            'node_modules',
        ]
        transform: require('css-whitespace')
    }))
    .toString();
```

### Options

#### encoding

Type: `String`
Default: `utf8`

Use if your CSS is encoded in anything other than UTF-8.

#### path

Type: `String|Array`
Default: `process.cwd()` or _dirname of [the rework source](https://github.com/reworkcss/css#cssparsecode-options)_

A string or an array of paths in where to look for files.
_Note: nested `@import` will additionally benefit of the relative dirname of imported files._

#### transform

Type: `Function`
Default: `null`

A function to transform the content of imported files. Take one argument (file content) & should return the modified content.
Useful if you use [`css-whitespace`](https://github.com/reworkcss/css-whitespace).

## What to expect

```css
@import "foo.css" (min-width: 25em);

body {
    background: black;
}
```

yields:

```css
@media (min-width: 25em) {
    body {
        background: red;
    }

    h1 {
        color: grey;
    }
}

body {
    background: black;
}
```

## License

MIT © [Jason Campbell](https://github.com/jxson) and [Kevin Mårtensson](http://github.com/kevva)

redpajama_set_name: RedPajamaGithub


text:
Grindr (/ˈɡraɪndər/) és una xarxa geosocial en format d'aplicació de mòbil enfocada cap a homes gais i bisexuals i persones trans, dissenyada per ajudar-los a conèixer altres homes i persones trans en la seva àrea. Està disponible tant en iOS com en  Android des de l' App Store i Google Play. Grindr consta d'una versió gratuïta i una de pagament en format de subscripció, anomenada Grindr Xtra.

L'aplicació fa servir la geolocalització i permet als usuaris descobrir els perfils propers. La interfície general d'usuari consta d'una graella que mostra les fotografies dels perfils, ordenats de menor a major distància de l'usuari. En clicar una de les fotografies, es mostra el perfil d'aquell usuari, com també l'opció per establir una conversa, enviar imatges, i la compartir la pròpia ubicació de manera precisa.

Grindr va ser la primera aplicació geosocial gai que es va llançar a l'iTunes App Store i des de llavors ha esdevingut l'aplicació per a mòbils gai més popular i amb la major comunitat del món. Actualment està disponible en 196 països.

Funcionament
La interfície del programa consisteix en un mosaic quadriculat de fotografies que ocupa la pantalla. Cada foto representa el perfil d'un home i estan ordenades segons la proximitat de la seva ubicació al moment. El perfil es crea accionant un botó de perfil que permet a l'usuari inserir ràpidament un pseudònim, una breu descripció, una sola fotografia de presentació i algunes dades personals bàsiques. Aquesta informació es mostra quan un usuari toca la miniatura de la foto que apareix a la graella incial. En aquell moment, la fotografia s'amplia i el perfil ocupa tota la pantalla, de manera que es mostren les dades de l'usuari i el seu estat de connexió. Des de la mateixa pantalla es pot optar per iniciar una conversa amb l'usuari, seleccionar-lo com a favorit o bloquejar-lo perquè l'aplicació no torni a mostrar aquest perfil. La pantalla de xat inclou la possibilitat d'enviar fotografies o la ubicació actual.

No es permeten fotos de nuus com a presentació de perfil. Això és degut al fet que Apple imposa als desenvolupadors d'aplicacions de iOS la distribució de material considerat pornogràfic.

Història
Grindr va ser llançat el 25 de març de 2009 per Proper Buddy Visor, LLC. Inicialment van començar a circular comentaris prudents però positius per la blogosfera gai a pàgines com  Queerty i Joe My God. Encara que va néixer als Estats Units, l'app va guanyar popularitat mundial gràcies al boca-orella i mitjans de comunicació diversos. El 18 de juny de 2012, Grindr va anunciar que havia arribat als 4 milions d'usuaris en 192 països arreu del món. A principis de 2018 arriba a 196 països i té 3.6 milions d'usuaris en línia diàriament. Més enllà dels EUA i Austràlia, el fundador Joel Simkhai ha informat d'activitat en països com l'Iran, l'Iraq i el Kazakhstan. El juliol de 2016, els Estats Units van aconseguir el major nombre d'usuaris amb 4,258,056, mentre que el 2015 Londres va coronar la llista de ciutats amb 698,252.

El gener de 2011, Grindr va guanyar el premi per "Millor aplicació de cites per a mòbil" als iDate Awards 2011. Grindr va anunciar el març de 2011 que estava desenvolupant una versió heterosexual anomenada temporalment Project Amicus. El 8 de setembre de 2011, Grindr va llançar Blendr, una aplicació similar per a persones de totes les orientacions sexuals, amb noves característiques que pretenien promoure amistats no sexuals.

El gener de 2012, Grindr va anunciar que era el guanyador del premi a "Millor aplicació de localització" dels TechCrunch's 2011 a la Cinquena Cerimònia Anual dels Crunchies Awards a San Francisco al Davies Symphony Hall Per altra banda, Grindr va ser nomenat el guanyador dels 2012 iDate Awards en dues de les 12 categories per a "Millor aplicació de cites per a mòbil" i "Millor nova tecnologia" a la novena edició de la Dating Industry & Internet Dating Conference a Miami. L'abril de 2012, Grindr va anunciar que els lectors de About.com havien triat Grindr com la "Millor app de cites" als 2012 About.com Readers' Choice Awards, amb el 74 per cent dels lectors que van escollir Grindr per damunt de Are You Interested, SKOUT, Tagged, Tingle and Zoosk.

L'agost de 2013, Grindr va llençar una versió actualitzada de l'aplicació que obligava als usuaris a registrar-se un compte. Els responsables van declarar que aquesta acció volia reduir el contingut brossa i millorar la portabilitat. La nova versió s'adaptava a la pantalla de l'iPhone 5, de manera que els usuaris dels nous dispositius iOS, com l'iPhone 5, ja no veiessin barres negres a sobre i a sota de la pantalla quan utilitzaven l'aplicació.

El 30 de setembre de 2013, Grindr va publicar la versió 2.0 per a iOS i Android. La interfície d'usuari va ser redissenyada i portava millores d'estabilitat, una nova característica de desplaçament (scrolling) infinit, imatges de la graella més grans i una safata de xat unificada. Grindr també va introduir un filtre anomenat Grindr Tribes, que permet als usuaris identificar-se per una de les diverses tribus dins del món gai i cercar, alhora, el seu tipus d'home. Les Grindr Tribes inclouen, en la seva nomenclatura en anglès: Bear, Clean-cut, Daddy, Discreet, Geek, Jock, Leather, Otter, Poz, Rugged, Trans and Twink. A part de les Tribes, els usuaris poden filtrar per edat i "buscant... ".

El 25 de març de 2014 pel cinquè aniversari de Grindr, l'aplicació havia aconseguit més de 10 milions de descàrregues i més de 5 milions d'usuaris actius mensuals arreu del món. El gener de 2016 Grindr va anunciar que havia vengut un 60% de participació de l'empresa a una empresa de videojocs xinesa, Pequín Kunlun Tech, per 93$ milions.

Grindr va assolir 27 milions d'usuaris el 2017.

Per tal de lluitar contra la difusió del VIH, Grindr va anunciar el març 2018 la introducció d'una nova funció que, en cas d'activar-se, envia un recordatori cada tres a sis mesos per a fer-se la prova del VIH. També ofereix la localització del local més proper per a la prova.

L'agost de 2018, l'empresa va decidir fer pública aquesta característica després de rebre l'aprovació l'empresa xinesa mare "Kunlun Grup".

Grindr per a la igualtat
El 2012, els operadors de Grindr van utilitzar el servei per distribuir "Grindr per a la Igualtat," informació geo-orientada sobre campanyes polítiques i la visió dels candidats en temes relacionats amb el col·lectiu LGTBI.

Controvèrsia i crítica

Problemes tècnics i de vulnerabilitat del programari
La versió d'Android de Grindr té un número substancial de crítiques negatives derivades d'errors no resolts, però ha augmentat a un 3.5 l'índex d'estrelles. L'agost de 2013, Grindr va llançar una actualització que obligava als usuaris a verificar els seus comptes mitjançant una adreça de correu electrònic vàlida i creant una contrasenya.

El gener de 2012, una vulnerabilitat de programari va exposar potencialment els detalls personals de centenars de milers d'usuaris. Grindr va emprendre accions legals en conseqüència i va efectuar canvis de programari per bloquejar la pàgina responsable de la filtració. Aquest lloc web va afectar un nombre petit d'usuaris, principalment australians, i roman tancat avui dia.

Triangulació potencial
L'agost de 2014, es va denunciar que les mesures relatives de distància de Grindr podien facilitar la triangulació dels usuaris i, per tant, mostrar la ubicació exacta d'individus. Es va dur a terme una prova per demostrar aquest concepte i es van poder realitzar més de 2 milions de deteccions en uns quants dies. Un client no autoritzat permet a qualsevol usuari registrat trobar la ubicació exacta d'un altre usuari. A causa de les protestes públiques de la comunitat LGTBI i els informes que la policia egípcia utilitzava Grindr per "caçar" persones homosexuals, Grindr va respondre desactivant la visualització de la distància a nivell global. El 10 de maig de 2015, es va reactivar la funció de distància, amb la possibilitat encara de triangular la posició d'un individu.
El maig de 2016, un grup de científics de la Universitat de Kyoto va demostrar a Andy Greenberg a la revista Wired com encara era possible localitzar precisament a algú, inclosos els usuaris que tinguessin la funció "mostrar distància" desactivada. L'equip d'investigadors va explorar un model d'atac nou anomenat "colluding-trilateration" mitjaçant el qual era possible localitzar qualsevol usuari de manera fàcil, barata i sense fer servir cap tècnica de hacking. El model d'atac no només funcionava amb Grindr però també amb Jack'd i "«Hornet»."., o qualsevol servei basat en localització que mostri fotos d'usuaris propers per ordre de proximitat.

Discurs ofensiu
Grindr ha estat criticada per no prendre suficients mesures per impedir la propagació de missatges ofensius, racistes i homofòbics per part d'alguns usuaris. El 2014, el creador de l'aplicació Joel Simkhai va contestar al diari israelià Haaretz sobre el tema del llenguatge ofensiu i racista a Grindr que "no li agradava però que tampoc era un professor de primària" i que "no era la seva feina fer de policia".

Problemes en la privacitat
L'abril de 2018, l'organització sense ànim de lucre noruega SINTEF va informar que els paquets de dades que Grindr cedia a tercers podien contenir l'estat de VIH dels usuaris. Aquest fet ha generat polèmica al voltant de Grindr a tot el món.

Censura
L'apliació està bloquejada en la seva totalitat o parcialment a Turquia, l'Iran, l'Aràbia Saudita i Indonèsia; i ha estat utilitzada per les autoritats d'Egipte per rastrejar i arrestar homes gais.

Venda de drogues
Grindr també ha estat objecte de polèmica pel fet que s'han trobat traficants de drogues oferint els seus productes a l'aplicació. Es poden trobar perfils on es ven marihuana, cocaïna, metamfetamines, GHB, i moltes més. L'app disposa de filtres per rastrejar aquestes paraules, però són fàcilment salvables a causa de l'argot utilitzat o les emoticones.

Vegeu també
 Homosocialització
 Tinder

Referències

Aplicacions mòbils

Homosexualitat masculina


Insert link around selected text/image?
I have made a plugin (based on an iFrame dialog) where a user can insert a link on the selected text.
It works great with text, but with images, nothing happens. Also, if the text has some formatting (e.g. bold), then it looses the formatting.
Does anyone know how to get the HTML instead of the plain text? So it would work with images too? I have looked at the ckeditor source, but couldn't find anything.
I was just trying to debug my issue, and somehow it just gave me what I wanted.
You really only need to see the link.setHtml line near the bottom. I tested IE9 (not IE10 as of this post), and then I tested Chrome and both worked. I haven't gone through a full test of Safari, FireFox, Opera, etc, but I'd say it's safe to use. Try it on your end and post a comment.
I could fix it on my code base too.


Most organizations struggle with communication. It is often listed as the number one problem executives have in leading their businesses. They struggle will silos, lack of clarity, disengagement, incomplete information, bottlenecks and more. These break downs cost organization millions of lost revenue each year. Managers are unable to get buy-in for change initiative so they are delayed. Customer feedback does not get to the people who can take action. Vision, mission, values and goals or poorly communicated often-leaving team members in the dark with little direction and motivation. New employees are quickly indoctrinated to the corporate communication practices and become disengaged.
We will provide a highly interactive process, which reveals your KCI's (key communication indicators). This process allows people to experience the realities of organizational communication and connect their different roles to situations and flows of communication. Each person will learn what choices and opportunities for improvement they have based on the different roles and situations (which chair am I in ?) they find themselves in. Participants will learn how they can immediately improve their own communication flow and improve productivity and engagement.
Description: Most leaders want to be true to who they believe they are. This can be a challenge if who you are conflicts with your leadership role. Many leaders struggle with authenticity when there is change or a new role, or when they have to sell themselves or handle feedback for improvement. You will learn how to have the success you desire without selling out. Participants become aware of the power of patterned emotional responses, and learn how to re-train their brain in order to develop more productive habits. Developing the ability to master oneself in moments of tension and stress creates new habits as well as building a foundation for personal and professional success. Participants develop their ability to focus on assertive communication skills and handle challenging behaviors, which are essential in achieving organizational objectives.
Become aware of the power of patterned emotional responses and continue to look for ways to interrupt unproductive behaviors.
Learn techniques to develop habits for improved results.
Manage conflict and challenging behaviors of others.
Enhance your ability to choose how you behave even in challenging or stressful situations.
This presentation is all about the stories we tell ourselves. We tell ourselves that we are certain "type" of person and that thinking keeps us stuck. When we understand there is a way to change the story in alignment with our attitudes and strengths, you will have greater motivation to change and achieve better results.


Credit sectors offer the best long-term opportunities in the fixed-income space, say BlackRock analysts. Investors can gain exposure to the area through high-yield and floating rate exchange traded funds.
"In the taxable fixed income space, we believe the best long-term opportunities can be found in the credit sectors of the market," according to a BlackRock research note.
Given the Fed's commitment to maintain loose monetary policies and to move forward with its quantitative easing program, yields on government securities will remain depressed at levels investors would not find appealing.
Additionally, investors may consider floating rate note ETFs to help against rising rates. Floating rate notes come with variable coupons. The coupon rates are periodically adjusted, which help protect against capital erosion in a rising rates environment.
For more information on fixed-income options, visit our bond ETFs category.


With over thirty nine years experience in the garden & leisure building industry we can easily spot the difference between a good quality office building and an exceptional one and we positively refuse to lower our standards. You can find cheaper garden rooms but you won't find better for delivery to Farnham including modern, smart and insulated buildings. All of our partners have been carefully chosen to offer the finest selection of buildings, with the best after-sales service, at the very best prices.
A television program set in Buckinghamshire had a garden room has its main star. The Buckingham Advertiser, the local paper, reported that a 10 part TV show would be filmed in the shed in an Amersham Garden. Jamie Malden, the locally retired headmistress devised the idea for the program which was called Taking Threads.
The program profiled local artists as well as featuring textile art. The 52-year-old Jamie Malden told the newspaper that she was a Blue Peter child and absolutely loved the idea of making things and was always collecting washing up bottles to use later. She went on to say that she thought she has found her calling and that she hoped to spread the 'joy of stitch' through the programs.
The series was filmed in her garden room and some of the interviewees included Myfanwy Hart, Gilda Baron, Di Wells and Angie Hughes among many others. Talking Threads was not the 1st TV show to feature garden sheds in the program and I think in Burgess Hill. Channel 4's Big Breakfast program used to have a regular feature from Trevor Baylis's workshop set in his garden. This program finished a number of years ago.
Trevor Baylis who was born in 1937 is an English inventor. His best-known invention was the wind-up radio which was a godsend to people in Africa and helped to get information about Aids to its people. The radio worked by the user winding a crank which created energy which drove an electrical generator powering the radio.


text:
Benjamin Brian Thomas Watt owner-founder of Buzzin' Fly Records and Strange Feeling Records is a British musician, DJ, and record producer, best known as one half of the duo, Everything but the Girl.
Watt began recording in 1981 on the indie label Cherry Red - and went on to make the album North Marine Drive, a collection of folk-jazz solo recordings in 1983. He then joined forces with vocalist Tracey Thorn. For 18 years they wrote and recorded together - creating nine studio albums as Everything but the Girl (EBTG), signing to Warners in 1984, and then Virgin in 1995. These albums and many of their singles achieved UK and US chart success, the song "Missing" reaching number two on the U.S. Billboard Hot 100 in 1995. In the mid-nineties, the band shifted focus from alt-pop towards electronica, charting with Walking Wounded, Protection (with Massive Attack), Temperamental and other work.
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redpajama_set_name: RedPajamaCommonCrawl


text:
A voice from inside the Church of Scientology: Yes, the 'Survival Rundown' drives you insane - 2015-05-08
A voice from inside the Church of Scientology: Yes, the 'Survival Rundown' drives you insane May 8, 2015, Tony Ortega, Underground Bunker
Over the past couple of weeks, we've been posting segments from a secretly-recorded audiotape that captures a Sea Org executive, Andres Rodriguez, talking to a group of Scientologists about their courses. We've posted three portions of the recording so far — part 1, part 2, part 3.
The tape gives us a rare glimpse inside a Scientology "org" and what it's like to face the challenges of the "Bridge to Total Freedom."
In particular, we hear Rodriguez complain about the way students have been cutting corners in the "Survival Rundown," a set of processes that have been given special emphasis by Scientology leader David Miscavige. Although they occur relatively early in a Scientologist's career, many high-level members have been asked to take or retake the "SRD." As we reported recently, one of our sources inside the church told us that all of his friends who were "OT 8's" — the highest achievement on the Bridge, which can take half a million dollars or more to reach — were now working through the SRD.
{{cite news | author = Tony Ortega | title = A voice from inside the Church of Scientology: Yes, the 'Survival Rundown' drives you insane | url = https://tonyortega.org/2015/05/08/a-voice-from-inside-the-church-of-scientology-yes-the-survival-rundown-drives-you-insane/ | work = Underground Bunker | date = May 8, 2015 | accessdate = August 21, 2017 }}
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Andres Rodriguez
Bridge to Total Freedom
Case Supervisor
Chris Shelton
End Phenomena
Objective Process
Purification Rundown
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Tony Ortega
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text:
Bus driver hides inside goods trailer while trying to escape arrest over fatal accident
By Naledi Shange
Image: Supplied by SAPS The scene of a deadly bus crash in Polokwane which claimed the lives of nine people.
The driver involved in a tragic bus accident on the N1 in Limpopo' which claimed the lives of nine passengers' will remain behind bars' police said on Wednesday.
He appeared in court on Tuesday after he was caught trying to flee the country over the long weekend. Colonel Moatshe Ngoepe named the man as George Themba – aged 41. He is from Zimbabwe. Ngoepe said Themba appeared before the Polokwane Magistrate's Court' where he was charged with nine counts of culpable homicide and another charge of reckless driving.
"He was denied bail and his cases were postponed to 2 October 2018 for further police investigations'" Ngoepe said.
The deadly accident happened last Friday.
Limpopo bus crash driver caught trying to flee SA
"It is alleged that the bus was travelling from the direction of Polokwane towards Gauteng province when the driver lost control and it overturned. The bus was carrying 61 occupants' including the driver and the crew. Nine out of 61 were certified dead at the scene. The 52 other injured people including Themba were taken to different hospitals for medical treatment'" Ngoepe said.
"As the process of intensive investigations by the police was unfolding' especially on the possible cause of that accident' he disappeared following his discharge from hospital and fled towards the Beit Bridge port of entry. The police were then tipped off' they swiftly responded and subsequently' the driver was caught hidden inside the goods trailer' trying to illegally cross the border to Zimbabwe'" he added.


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text:
Health officials seek answers to Saratoga Springs sickness
By Jed Boal | Posted - May 17, 2010 at 10:14 p.m.
SARATOGA SPRINGS -- Saratoga Springs lifted its drinking water boil order Saturday, but people are still getting sick, and at least one person plans to sue the city.
Many residents are frustrated and still afraid to drink the water.
"We've been sick for a week," says Elizabeth Harmer.
She and her husband, and three of their four kids, have been sick with nausea, vomiting and stomach problems. The sickness started in her family more than a week ago, and she has neighbors who just got ill Monday.
"I don't know how much longer it's going to last, but we've all been sick," Harmer says.
Until Monday, she was upset with the lack of official information, but the county health department has now updated its website with the latest detail.
The Utah County Health Department and the state say the water is safe, but they still need to pinpoint the source of the bacterial outbreak that has sickened many.
A woman named Niki Diaz, through her lawyer, notified the city she plans legal action for the sickness that sent her to the emergency room. According to her attorney's statement, she continues to need medical care as she recovers from her campylobacter infection.
Health officials issued the boil water order Thursday and lifted it Saturday after chlorinating the system.
The city continues to work with the county and state health departments and the Utah Division of Drinking Water to get to the bottom of the problem.
"We're trying to be cautious," says Saratoga Springs City Manager Ken Leetham. "The water is safe to drink."
The Utah County Health Department counts 15 lab confirmed cases of campylobacter but cannot confirm the source. Officials still think water is the likeliest common link. Dozens, maybe hundreds more are sick, but did not go to a doctor.
Dr. Joseph Miner, the Executive Director of the Utah County Health Department says many of the ill likely got sick after one person in the house was sickened by the water and spread it to others.
"Individuals who have this kind of illness should not prepare food for others in the family, because that is a risk no matter how well you wash your hands," Miner says.
If people continue to get sick after chlorinating in the system, that may lead health investigators in a different direction.
"That's one thing we'll be looking for: new cases which are continuing to occur even though the water has been chlorinated, or once they discontinue chlorinating the water," Miner says.
As health specialists search for the source, Miner says the outbreak coincides with the city turning on the pressurized irrigation system. If someone working on both water lines mixed them up, that could lead to bacterial contamination.
"That's called a cross-connection, and that contaminated irrigation water can get into the public drinking water system," Miner says.
The city is looking into new installations and construction on water lines to see it that's how the bacteria got into the system.
Five deep wells supply the water and are considered protected. For that reason, Saratoga Springs does not regularly chlorinate the water unless there's an emergency like this.
"We're going to continue to chlorinate the system until we can locate the source of any bacteria that may have caused these illnesses," Leetham says.
The city manager says they may consider a chlorinating system to prevent these problems in the future, and the executive director of the health department recommends it.
Residents just hope it ends soon.
"It's uncomfortable," Harmer says. "It's sick. You don't want to go on not knowing how long that's going to last."
The health department plans to update its outbreak website daily.
E-mail: jboal@ksl.com
Utah County campylobacter investigation website
More illness reported in Saratoga Springs
Jed Boal


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