text:
\section{Introduction}

The small-scale low-ionization structures (LIS) of planetary nebulae were
classified in terms of their morphology and kinematics by Gon\c calves, Corradi
\& Mampaso (2001) as knots, jets and
jetlike\footnote{These are features whose morphology resemble highly supersonic jets, but that
share the expansion of the nebular components in which they are embedded.} systems,
either in pairs or isolated. From this, and subsequent works (e.g. \citealt{g2004}, and  references therein)
it has became apparent that: i) around 10\% of the Galactic PNe
are known to possess LIS; ii) they are indistinctly spread among all the PNe
morphological classes; iii) 50\% of these PNe have highly collimated,  high-velocity
jets, and/or  high-velocity pairs of knots (FLIERs; fast, low-ionization emission
regions, \citealt{bea1993});
and iv) most of them are mainly photoionized.

However, a number of key questions remain open: are there significant density contrasts
between LIS and the higher ionization main components (rims, attached shells and detached
haloes) of the nebula? What are the typical electron densities of the different
types of LIS?

We are involved in a long-term project for characterizing the
small-scale LIS of PNe since they can tell
us much about the formation and evolution of PNe. The main issues we
can access by studying the LIS are:

\begin{enumerate}
\item the collimation processes of LIS in regard to those processes responsible
for the shape of the PN itself, or the mass-loss processes during the AGB and
post-AGB phases;

\item the effect of the ionization front on the fossil AGB features; and

\item the role of disks and magnetic fields in shaping the highly
collimated outflows (jets) in PNe.
\end{enumerate}

Our motivation for the present analysis is to go a step further on
the study of the different LIS analyzing their densities. LIS can move through their
environments either with high or low velocity. In the first case (the so-called FLIERS),
radial velocities of $24-200$~\relax \ifmmode {\,\rm km\,s}^{-1}\else \,km\,s$^{-1}$\fi with respect to the PN main components are typically measured
\citep{bea1993}, whereas in the second instance (the SLOWERs, slow moving low-ionization emission
regions; see \citealt{p2000}) the knots
do not show peculiar velocities and share the typical 30~\relax \ifmmode {\,\rm km\,s}^{-1}\else \,km\,s$^{-1}$\fi\ (for elliptical shells)
to 100~\relax \ifmmode {\,\rm km\,s}^{-1}\else \,km\,s$^{-1}$\fi\ (for bipolar lobes) expansion velocities of their host PNe.
A straightforward question arises from this:
how is the density contrast between the LIS and rims, shells or haloes
correlated with the different velocity regimes?

In this paper we analyse 4 PNe that contain pairs of knots, either
of high- or low-velocities.

We present our spectroscopic data and treatment, in Section~2. The line
fluxes obtained for as many as possible large- and small-scale
components of the four PNe, and the derived physical properties
for each of the components are shown in Sections 3 to 6. Finally,
Section 7, is dedicated to the discussion of the results in terms of
the match with the theoretical model predictions, and to our concluding remarks.

\section{Observation and Data Treatment}

\begin{table}
 \caption{Log of the INT+IDS observations}
\begin{tabular}{lcc}
\hline
PN Name and P.A. & Obs. Date & Exposure (s)\\
 &  & 3$\times$ \\
\hline
He~1-1\ - 315$^\circ$\  & Aug 31 & 300, 2400	   \\
IC~2149\ - 70$^\circ$\   & Sep 01 & 300, 900, 1800 \\
KjPn~8\ - 98$^\circ$\   & Aug 30 & 1200           \\
KjPn~8\ - 120$^\circ$\  & Aug 30 & 300, 1200      \\
NGC~7662\ - 175$^\circ$\ & Sep 05 & 60,  300       \\
NGC~7662\ - 248$^\circ$\ & Sep 04 & 30,  60,  300  \\
\hline
\end{tabular}
\label{LOG}
\end{table}

A 120 sec exposure  H$\alpha$\ + [N {\sc ii}]\ (6568/95{\AA}) image of He~1-1\ (Figure~\ref{i_he11})
was retrieved from the IPHAS database (INT/WFC Photometric H$\alpha$\ Survey of the Northern
Galactic Plane: http://www.iphas.org).
We also retrieved from the Hubble Space Telescope (HST) Archive two WFPC2 images of
IC~2149: the V-band (filter 555W, 2 sec exp. time) and the [O {\sc iii}]\ (F502N, 100 sec) images,
obtained on 1995 (proposal 6119), see Figure~\ref{i_ic2149}. The [N {\sc ii}]\ (F658N, 400 sec)
image of NGC~7662\ (Perinotto et
al. 2004; Figure~\ref{i_ngc7662}), was also retrieved from the HST archive, and was obtained
on 1996. The image of KjPn~8\ was obtained with the
2.5-m Nordic Optical Telescope (NOT) at the Observatorio del Roque de
los Muchachos (European Northern Observatory, La Palma, Spain), with
ALFOSC camera, in June 26, 2002. The image we show in
Figure~\ref{i_kjpn8} is the result of one exposure of 1 800~s through
the narrow-band filter \nii6584\AA.

Spectra of the 4 PNe were obtained on August 31 and September 1, 4 and
5 of 2001, at the 2.5 m Isaac Newton Telescope (INT) at the Observatorio del
Roque de los Muchachos using the Intermediate Dispersion Spectrograph (IDS). The 235
mm camera and the R300V grating were used, providing a spectral
coverage from 3650 to 7000~\AA\ with a spectral reciprocal dispersion
of 3.3~\AA~pixel$^{-1}$. The spatial scale of the instrument was
0\farcs70~pixel$^{-1}$, with the TEK5 CCD. Seeing varied from
0\farcs9 and 1\farcs1.
The slit width and length were 1\farcs5 and
4~\arcmin, respectively. These data were taken with the slits
positioned through the centre of the nebulae at the position angles
(P.A.), and with exposure times given in Table~1. Each of the
exposures was taken 3 times, as listed in the table. The longer
exposures were used to measure the fluxes of most emission
lines. However, for almost all the PNe, the
[O {\sc iii}]$\lambda\lambda$~4959,5007~{\AA}, the
[N {\sc ii}]$\lambda\lambda$~6548,6583~{\AA} doublet as well as the H$\alpha$\ and even
the H$\beta$\ lines were saturated at the brightest features in the longer
exposures, thus, the shorter exposures where used in these
cases.
Differently of the way we took long-slit spectra of the
other PNe, in the case of KjPn~8\ the slit was centred on the position
of the central star, and then it was shifted in order to cover
each of the knots. Compared to the weather conditions during the
observation of the other three PNe, that of the KjPn~8\ was poor
(clouds appeared during the integration).

During the night, bias frames, twilight and tungsten flat-field exposures, wavelength calibrations,
and exposures of standard stars (BD +332642, Cyg OB2 No. 9, HD 19445, and BD +254655) were
obtained. Spectra were reduced following the IRAF instructions for long-slit spectra, being
bias-subtracted, flat-fielded, combined in order to improve the signal-to-noise ratio (S/N) and
eliminate cosmic rays, wavelength-calibrated, and sky-subtracted. Finally, they were flux-calibrated
using the above mentioned standard stars and the mean atmospheric extinction curve for La Palma.

\section{He 1-1}

\begin{figure}
\begin{center}
 \psfig{file=drg_fig1_a.eps,width=7.0truecm}
 \psfig{file=drg_fig1_b.eps,width=7.0truecm}
\end{center}
\caption{He~1-1: IPHAS H$\alpha$+[N {\sc ii}]\ image. The 3 structures under analysis are
  indicated in the image.

  The size of the extraction windows in the spectra includes 4\farcs2 each
  side from the centre for the Rim, and extends from + 4\farcs9 to
  7\hbox{$^{\prime\prime}$}, and from -4\farcs9 to -7\farcs7 from the centre, for the
  SE and the NW knots respectively. The extraction window for the
  entire portion of the nebula covered by the slit, NEB, extends along 14\farcs7.}
 \label{i_he11}
\end{figure}

PN G055.3+02.7 (He~1-1) is a point-symmetric PN with a pair of
low-ionization knots.  See in Figure~\ref{i_he11} the extensions of
its bright Rim (or a combination of a rim and a shell), the large-scale
component that dominates the emission
of the nebula, and the SE and NW strings of knots, which correspond to
the small-scale faint structures seen in the [N {\sc ii}]\ NOT image.

In the uppermost part of Table~2
we list selected line
fluxes of the Rim, the knots and the entire portion of the nebula
covered by the slit. These include all the electron density and
temperature diagnostic emission lines covered by the IDS
spectra. Absolute H$\beta$\ fluxes, F$_{{\rm H}\beta}$, integrated along
the slit for each nebular component are also given in Table~2.
The Balmer lines ratios (H$\alpha$/H$\beta$, H$\gamma$/H$\beta$\ and
H$\delta$/H$\beta$) were then used to derive the c$_{{\rm H}\beta}$, the
logarithmic ratio between observed and dereddened H$\beta$\ fluxes. For the
derivation of $c_{\rm H\beta}$, we assumed $T_{\rm e}$ = 10$^4$~K and the
densities given by the [S {\sc ii}]\ ratio of each region. Theoretical Balmer
line ratios from \citet{of2006} and the reddening law of
\citet{ccm1989} were used. The weighted average of $c_{\rm H\beta}$, per PN
component, is the one given in the table.  $c_{\rm H\beta}$\ is constant
along the slit, and the $c_{\rm H\beta}$=1.49$\pm0.16$ for the entire nebula is
lower than the value previously published by \citet{tea1992}. The
latter authors found a range of values for $c_{\rm H\beta}$, which goes from 1.9
to 2.2. Note, however, that their values are based only on the
H$\alpha$/H$\beta$\ ratio. Fluxes were then dereddened using the derived
$c_{\rm H\beta}$. The dereddened fluxes, or intensities, are not shown in the
table. Instead, figures in the table correspond to the observed
fluxes.

\begin{table}
\centering
\begin{minipage}{90mm}
{\scriptsize
\caption{He~1-1: Observed line fluxes, flux errors, $c_{\rm H\beta}$, N$_e$\ and T$_e$.}
\begin{tabular}{lcccc}
\hline
\hline
Line ID & \multicolumn{1}{c}{Rim} & \multicolumn{2}{c}{Knots} &
\multicolumn{1}{c}{NEB} \\
       & & SEk & NWk  & \\
\hline
\noalign{\smallskip}
{}[S{\sc ii}] 4072.0     & 6.232   & -      & -      & 6.464 \\
H$\delta$ 4101.8         & 15.57   & -      & -      & 15.97 \\
H$\gamma$ 4340.5         & 29.69   & -      & -      & 29.13 \\
{}[O{\sc iii}] 4363.2    & 11.36   & 16.89  & 14.61  & 13.04 \\
H$\beta$ 4861.3          & 100.0   & 100.0  & 100.0  & 100.0 \\
{}[O{\sc iii}] 4958.9    & 543.4   & 587.7  & 601.7  & 566.8 \\
{}[O{\sc iii}] 5006.86   & 1715.   & 1773.  & 1808.  & 1774. \\
{}[CL{\sc iii}] 5517.7   & 3.321   & 22.56  & 15.57  & 4.152 \\
{}[CL{\sc iii}] 5537.9   & 3.041   & 18.23  & 13.04  & 3.640 \\
{}[N{\sc ii}] 5754.6     & 11.90   & 23.46  & 24.87  & 13.83 \\
{}[N{\sc ii}] 6548.0     & 319.2   & 480.6  & 413.9  & 335.1 \\
H$\alpha$ 6562.8         & 993.9   & 977.6  & 981.2  & 1021. \\
{}[N{\sc ii}] 6583.4     & 1034.   & 1436.  & 1321.  & 1075. \\
{}[S{\sc ii}] 6716.5     & 129.3   & 114.4  & 124.4  & 132.3 \\
{}[S{\sc ii}] 6730.8     & 169.6   & 114.7  & 139.2  & 172.1 \\
\\
F$_{{\rm H}\beta}$ $^a$  & 21.62         & 0.4565        & 0.6247        & 22.37 \\
c$_{{\rm H}\beta}$       & 1.46$\pm$0.20 & 1.44$\pm$0.32 & 1.45$\pm$0.33 & 1.49$\pm$0.16 \\
\\
 & \multicolumn{4}{c}{Percentage errors in line fluxes} \\
\\
(0.01--0.05)H$\beta$\  &35  &52   &60   &31 \\
(0.05--0.15)H$\beta$\  &15  &25   &27   &13 \\
(0.15--0.30)H$\beta$\  &11  &20   &20   &11 \\
(0.30--2.0)H$\beta$\   &10  &17   &16.5 &8.5\\
(2.0--5.0)H$\beta$\    &9.5 &15   &16   &6.5\\
(5.0--10.0)H$\beta$\   &9   &14.5 &16   &6.5\\
$>$ 10H$\beta$\         &9   &14.5 &16   &6.5\\
\\
& \multicolumn{4}{c}{Electron Densities (cm$^{-3}$) and Temperatures (K)} \\
\multicolumn{4}{l}{}\\
N$_e$[S {\sc ii}]   	& 1600$\pm$230   & 600$\pm$140    & 900$\pm$210    & 1550$\pm$190   \\
N$_e$[Cl {\sc iii}] 	& 1700$\pm$830   & 800$\pm$230    & 1000$\pm$330   & 1350$\pm$580   \\
T$_e$[O {\sc iii}]        & 12500$\pm$2060 & 14400$\pm$3320 & 13450$\pm$4110 & 13050$\pm$1580 \\
T$_e$[N {\sc ii}]         & 10800$\pm$1800 & 12900$\pm$2980 & 14000$\pm$3320 & 11400$\pm$1590 \\
T$_e$[S {\sc ii}]         &  8750$\pm$1450 & -              & -              &  9300$\pm$1350 \\
\hline
\hline
\multicolumn{5}{l}{{\bf $^a$} In units of 10$^{-15}$erg cm$^{-2}$ s$^{-1}$} \\
\end{tabular}
}
\end{minipage}
\label{t_he11}
\end{table}

The middle part of Table~2
shows the errors on the
fluxes. They were calculated taking into account the statistical errors
in the measurements, as well as systematic errors of the
flux calibrations, background determination, and sky
subtraction.

In the lowermost part of Table~2
electron densities and temperatures are presented. At least two different
measures of T$_e$\ and N$_e$\ are available for each PN component. They
represent regions of low (N$_e$[S {\sc ii}], T$_e$[N {\sc ii}]\ and T$_e$[S {\sc ii}]) and medium
excitation (N$_e$[Cl {\sc iii}]\ and T$_e$[O {\sc iii}]).

The density of the nebula can be compared with \citet{skas1992}.  They
find N$_e$[S {\sc ii}]=1.19$\times$10$^3$~cm$^{-3}$, in moderate agreement with
ours. Figures for T$_e$\ and N$_e$\ of the knots were previously published
only in a proceeding contribution by \citet{benitez02}: 11~300~K for
the temperature of the NW knot, and densities of 300~cm$^{-3}$ and
600~cm$^{-3}$, for the SE and NW knots respectively.  These values
hardly agree with ours. Note that they did not derive, but assumed
the 10$^4$~K of the SE knot.

Figure~\ref{td_mosaic} (top left panel) and Table ~2 shows that both
density measurements in each region of the nebula are equal
within the errors, whereas N$_e$\ of the Rim is higher than that of the
SE and NW knots, by factors of $\sim$2.7 and $\sim$1.8,
respectively.
There is a good agreement between the two temperature
diagnostics obtained for the three PN components.

Figure~\ref{td_mosaic} shows that T$_e$\ at the centre could be somewhat lower
than at the knots, but the variation is within the errors.

Summarising, the pair of knots in He~1-1\ are substantially less dense
than the Rim, whereas no strong evidence exist for significant temperature
variations from the Rim to the knots.

\begin{figure*}
\psfig{file=drg_fig2.eps,width=16.0truecm}
\caption{Electron densities and temperatures as a function of the distance to the centre of
the nebula. The different structures under analysis are shown as symbols that correspond
to the centre of each structure, as defined in the images (Figures~1, 3, 4, and 5). Filled
(N$_e$[S {\sc ii}]) and open (N$_e$[Cl {\sc iii}]) triangles represent densities, while filled (T$_e$[N {\sc ii}]) and open
(T$_e$[O {\sc iii}]) circles, as well as the filled box (T$_e$[S {\sc ii}]) represent electron
temperatures. Symbols
are plotted slightly displaced in distance in order to avoid overlapping. Horizontal lines
represent  densities and temperatures averaged along the slit (NEB): continuous line for N$_e$[S {\sc ii}], large-small
dashed line for N$_e$[Cl {\sc iii}], small dashed line for T$_e$[O {\sc iii}], medium dashed line for T$_e$[N {\sc ii}],
and large dashed line for T$_e$[S {\sc ii}].
TOP LEFT: He~1-1\ -  from left to right the NW knot, the Rim and the SE knot, respectively,
as in  Figure~\ref{i_he11}.
BOTTOM LEFT: IC~2149\ - From left to right, the NE knot,
the Core and the SW knot as in Figure~\ref{i_ic2149}.
TOP RIGHT: NGC~7662\ -
 P.A.=175$^{\circ}$; five zones of the Inner rim and Outer shell, as shown in Figure~\ref{i_ngc7662} and Table~5.
 BOTTOM RIGHT:NGC~7662\ -
 P.A.=248$^{\circ}$; further five zones of the Inner rim and FLIERs, following Figure~\ref{i_ngc7662}
 and Table~5.
  }
\label{td_mosaic}
\end{figure*}

\section{IC 2149}

\begin{figure}
\psfig{file=drg_fig3.eps,width=8.0truecm}
 \caption{IC~2149: HST 555W (V) image. Since this filter is centred in [O {\sc iii}], only the Core
 is clearly identified in this image. The low-ionization NEk and its fainter SWk counterpart
 are hard to see in this image, but are easily identified in the [N {\sc ii}]\ image in Fig.1 of
 \citet{vel2002}.
 The spectroscopic sizes of the Core, NE  and SW knots are, respectively: 2\farcs1
 each side from the centre; - 2\farcs8 to - 8\farcs4; and + 2\farcs8 to 6\farcs3.
 The entire PN, NEB, is 14\farcs7 in size.}
 \label{i_ic2149}
\end{figure}

\begin{table}
\centering
\begin{minipage}{90mm}
{\scriptsize
\caption{IC 2149: Observed line fluxes, flux errors, $c_{\rm H\beta}$, N$_e$\ and T$_e$}
\begin{tabular}{lcccc}
\hline
\hline
Line ID & \multicolumn{1}{c}{Core} & \multicolumn{2}{c}{Knots} &
\multicolumn{1}{c}{NEB}\\
       & & NEk  &  SWk  &  \\
\hline
\noalign{\smallskip}
{}[S{\sc ii}] 4072.0     & -      & 5.743  & 5.625 & 3.011 \\
H$\delta$ 4101.8         & 15.75  & 26.99  & 36.27 & 24.14 \\
H$\gamma$ 4340.5         & 40.46  & 43.41  & 61.99 & 46.12 \\
{}[O{\sc iii}] 4363.2    & 3.838  & 2.457  & 5.333 & 3.850 \\
H$\beta$ 4861.3          & 100.0  & 100.0  & 100.0 & 100.0 \\
{}[O{\sc iii}] 4958.9    & 180.1  & 124.5  & 140.7 & 150.9 \\
{}[O{\sc iii}] 5006.86   & 540.2  & 378.4  & 408.4 & 454.0 \\
{}[CL{\sc iii}] 5517.7   & -	  & 0.367  & 0.545 & 0.386 \\
{}[CL{\sc iii}] 5537.9   & - 	  & 0.516  & 0.481 & 0.440 \\
{}[N{\sc ii}] 5754.6     & 1.140  & 1.633  & 1.227 & 1.299 \\
{}[N{\sc ii}] 6548.0     & 15.03  & 30.27  & 18.55 & 22.06 \\
H$\alpha$ 6562.8         & 320.6  & 321.3  & 277.8 & 315.1 \\
{}[N{\sc ii}] 6583.4     & 43.07  & 91.54  & 51.81 & 65.23 \\
{}[S{\sc ii}] 6716.5     & 1.288  & 3.201  & 2.418 & 2.261 \\
{}[S{\sc ii}] 6730.8     & 2.312  & 5.607  & 3.385 & 3.860 \\
\\
F$_{{\rm H}\beta}$ $^a$  & 11.17     & 12.78          & 4.549 & 31.76 \\
c$_{{\rm H}\beta}$       & 0.07$^b$  & 0.14$\pm$0.015 & 0.00  & 0.12$\pm$0.008 \\
\\
 & \multicolumn{4}{c}{Percentage errors in line fluxes} \\
\\
(0.01--0.05)H$\beta$\  &17   &24  &39  &10  \\
(0.05--0.15)H$\beta$\  &10   &17  &24  &5.5 \\
(0.15--0.30)H$\beta$\  &7    &11  &16  &4.5 \\
(0.30--2.0)H$\beta$\   &6.5  &8   &10  &4.5 \\
(2.0--5.0)H$\beta$\    &5.5  &7   &8.5 &4.5 \\
(5.0--10.0)H$\beta$\   &4.5  &6.5 &7   &4   \\
$>$ 10 H$\beta$\       &4.5  &6   &6.5 &4   \\
\\
& \multicolumn{4}{c}{Electron Densities (cm$^{-3}$) and Temperatures (K)} \\
\multicolumn{4}{l}{}\\
N$_e$[S {\sc ii}]           & 6050$\pm$1450  & 5350$\pm$1550  & 2050$\pm$1130 & 4650$\pm$660 \\
N$_e$[Cl {\sc iii}]         & -              & 7600$\pm$2750  & 1500$\pm$870  & 4000$\pm$680  \\
T$_e$[O {\sc iii}]          & 10350$\pm$1760 & 10150$\pm$2560 &12700$\pm$3150 & 11050$\pm$1170 \\
T$_e$[N {\sc ii}]           & 12300$\pm$2150 & 10450$\pm$2600 &12350$\pm$4850 & 11000$\pm$1170 \\
\hline
\hline
\multicolumn{5}{l}{{\bf $^a$} In units of 10$^{-14}$erg cm$^{-2}$ s$^{-1}$} \\
\multicolumn{5}{l}{{\bf $^b$} This c$_{{\rm H}\beta}$ values is the average between the knots' values; see text.} \\
\end{tabular}
}
\end{minipage}
\label{t_ic2149}
\end{table}

PN G166.1+10.4 has an apparent shape that does not easily compare
with the classification bins (round, elliptical, bipolar or
quadrupolar, irregular and point-symmetric) usually adopted for
PNe. Kinematic modelling suggests that it is a bipolar PN
(\citealt{vel2002}; \citealt{fhl1994}; \citealt{zk1998}).  As shown in Figure~\ref{i_ic2149},
IC~2149\ is composed by a bright higher
ionization emission zone, the Core, and by a pair of lower excitation
knots, the North-Eastern one being much brighter than its
counterpart to the South-West. In fact only
the two former structures can be identified from
Figure~\ref{i_ic2149}. Please refer to Fig.1 of \citet{vel2002}, in
which not only a higher excitation image is show, but also the lower
excitation [N {\sc ii}]\ and [S {\sc ii}]\ are presented.  In their [N {\sc ii}]\ image the SW LIS is also clearly seen.

Table~3
contains the spectroscopic results for IC~2149, obtained from the INT+IDS
spectra at P.A.=70$^\circ$\ (observed and absolute H$\beta$\ fluxes, flux errors, $c_{\rm H\beta}$,
N$_e$\ and T$_e$) for the Core and pair of LIS of the nebula.

The H$\alpha$/H$\beta$\ ratio was used to obtain the $c_{\rm H\beta}$\ of the NEk, SWk
and NEB regions. Owing to the presence of Balmer line absorption in
the central zones \citep{vel2002}, the $c_{\rm H\beta}$\ of the Core was adopted
as the average from the knots' values. The value measured for the
nebula $c_{\rm H\beta}$=0.12$\pm0.01$ is in agreement with other published values
(\citealt{fhl1994}; \citealt{ciardullo1999}), but it is much smaller
than the value (0.41) obtained by \citet{vel2002} for the Core and the knots.

The gas physical conditions we derived to this PN (Table~3 and left bottom panel
of Fig.~2) compare relatively well with those derived by
\citet{vel2002} for the North-Eastern knot and for the NEB. The
exception is the N$_e$[S {\sc ii}], for which they obtained values of 10~000 and
9~600~cm$^{-3}$ while we found 5~350$\pm$1~550 and
4~650$\pm$660~cm$^{-3}$, for the NEk and NEB, respectively. We cannot
understand the reason of this discrepancies, since they do not depend
on the very different $c_{\rm H\beta}$\ applied to correct the fluxes. On the
other hand, the T$_e$\ that would be affected by our different choices
in terms of $c_{\rm H\beta}$, are in reasonable agreement with theirs (see
\citealt{vel2002} Table~1).  If only NEB is concerned, our results
also agree with the results obtained by \citet{fhl1994}.

As [Cl~III] $\lambda\lambda$5517,5537\AA\ were not detected, only
N$_e$[S {\sc ii}]\ could be derived for the Core.  Figure~\ref{td_mosaic} shows
that the two density diagnostics for each of the knots are such that
SWk (N$_e$[S {\sc ii}]=2~050$\pm$1~130) is significantly less dense than NEk,
whose density is similar to that in the Core (N$_e$[S {\sc ii}]=5~350$\pm$1~550 and
6~050$\pm$1~450, respectively).

In spite of an apparent increase of T$_e$[O {\sc iii}]\ and T$_e$[N {\sc ii}]\ from the
North-Eastern to the South-Western side of the nebula, variations
are within the errors.

\section{KjPn~8}

PN G112.5-00.1 (KjPn~8) is a huge PN (size $\sim$ 14~\arcmin $\times$
4~\arcmin; L\'opez, V\'azquez \& Rodr\'\i guez 1995) with multiple
polar ejections.  A number of papers  deal with the
characteristics of this PN, including: i) narrow-band imaging of its
many structures in the different scales, \citet{lvr1995}; ii) proper
motions of its latest bipolar ejections, \citet{M1997}; iii) kinematics
of the large bipolar lobes and of the pair of knots,
\citet{lmbr1997}; and iv) temperature, density and chemical abundances of
the inner nebula, V\'azquez, Kingsburgh \& L\'opez (1998). At much
smaller scales, a ring that seems to collimate the many structures
(with its CO and H$_2$ counterpart) has been detected giving support to
the idea that KjPn~8\ had two PNe-like events in its history
(\citet{lea2000}). However, N$_e$\ and T$_e$\ of its two pairs of
low-ionization knots were not properly measured so far, due to their
extreme faintness.

In our spectra only one of the knots of each pair could be measured with
a good S/N. At variance with the other PNe in our sample, no analysis of
the internal or entire nebula will be given, because of the huge extension
of the PN. Our results for the two SE knots of
KjPn~8\ are given in Table~4.

\begin{figure}
 \psfig{file=drg_fig4.eps,width=8.0truecm}
 \caption{KjPn~8: NOT [N {\sc ii}]\ image. The two P.A. of the structures under analysis
 are indicated in the image.
 The spectroscopic sizes of the two knots, SEk$_{98}$ is 14\hbox{$^{\prime\prime}$}\ and
 that of  SEk$_{120}$ is 10\farcs5.}
 \label{i_kjpn8}
\end{figure}

\begin{table}
\centering
\begin{minipage}{90mm}
{\scriptsize
\caption{KjPn8: Observed line fluxes, flux errors, $c_{\rm H\beta}$, N$_e$\ and T$_e$}
\begin{tabular}{lcc}
\hline
\hline
Line ID & \multicolumn{2}{c}{South Eastern Knots} \\
       & SEk$_{120}$  & SEk$_{98}$ \\
\hline
\noalign{\smallskip}
{}[S{\sc ii}] 4072.0      & 10.78 & 8.869 \\
H$\delta$ 4101.8          & 23.35 & 20.69 \\
H$\gamma$ 4340.5          & 41.41 & 42.54 \\
{}[O{\sc iii}] 4363.2     & 1.149 & 2.466 \\
H$\beta$ 4861.3           & 100.0 & 100.0 \\
{}[O{\sc iii}] 4958.9     & 100.5 & 101.8 \\
{}[O{\sc iii}] 5006.86    & 307.9 & 307.4 \\
{}[CL{\sc iii}] 5517.7    & -	  & 3.000 \\
{}[CL{\sc iii}] 5537.9    & -	  & 2.280 \\
{}[N{\sc ii}] 5754.6      & 9.351 & 12.95 \\
{}[N{\sc ii}] 6548.0      & 392.8 & 398.0 \\
H$\alpha$ 6562.8          & 438.8 & 453.3 \\
{}[N{\sc ii}] 6583.4      & 1191. & 1207. \\
{}[S{\sc ii}] 6716.5      & 99.79 & 98.28 \\
{}[S{\sc ii}] 6730.8      & 100.4 & 98.19 \\
\\
F$_{{\rm H}\beta}$ $^a$   & 2.468          & 1.221         \\
c$_{{\rm H}\beta}$        & 0.48$\pm$0.07  & 0.52$\pm$0.10 \\
\\
 & \multicolumn{2}{c}{Percentage errors in line fluxes} \\
\\
(0.01--0.05)H$\beta$\  & 30.5  & 42.5 \\
(0.05--0.15)H$\beta$\  & 22.5. & 34.5 \\
(0.15--0.30)H$\beta$\  & 15.5  & 27.5 \\
(0.30--2.0)H$\beta$\   & 10.5  & 16   \\
(2.0--5.0)H$\beta$\    &  8.5  & 10   \\
(5.0--10.0)H$\beta$\   &  6.5  & 8.5  \\
$>$ 10H$\beta$\        &  5    & 8.0  \\
\\
& \multicolumn{2}{c}{Electron Densities (cm$^{-3}$) and Temperatures (K)} \\
\multicolumn{2}{l}{}\\
N$_e$[S {\sc ii}]        & 600$\pm$90     & 600$\pm$140  \\
N$_e$[Cl {\sc iii}]      & -	        & 450$\pm$270	\\
T$_e$[O {\sc iii}]       & 9100$\pm$2960  & 11550$\pm$4950 \\
T$_e$[N {\sc ii}]        & 8500$\pm$1950  &  9550$\pm$3340 \\
T$_e$[S {\sc ii}]        & 9150$\pm$1250  &  8400$\pm$3010 \\
\hline
\hline
\multicolumn{3}{l}{{\bf $^a$} In units of 10$^{-14}$erg cm$^{-2}$ s$^{-1}$}\\
\end{tabular}}
\end{minipage}

\label{t_kjpn8}
\end{table}

When comparing our $c_{\rm H\beta}$\ values with those in the literature, particular care should be taken because they usually refer to different nebular regions, and reddening may vary along this large nebula.
\citet{vkl1998} measured very different $c_{\rm H\beta}$\ values for the three knots which they  labelled A1, A3 and B1: $c_{\rm H\beta}$\ $=$ 1.49, 0.96 and 0.56, respectively. Our $c_{\rm H\beta}$\ for
SEk$_{120}$ (their A1) is therefore 3 times smaller than
theirs, whereas for SEk$_{98}$ (their knot B1) both determinations agree very well, $c_{\rm H\beta}$=0.56 and 0.52$\pm0.10$,
respectively. The reason for the discrepant $c_{\rm H\beta}$\ in SEk$_{120}$ is not clear at present. As for the
density, they reported N$_e$[S {\sc ii}]=100~cm$^{-3}$ for both SEk$_{98}$ and SEk$_{120}$, while we
derived substantially larger values N$_e$[S {\sc ii}]=600$\pm$140 ([Cl {\sc iii}] = 450$\pm$270) and 600$\pm$90 for
SEk$_{98}$ and SEk$_{120}$, respectively.  The electron temperature in
the knots is measured in this paper for the first time.

Summarising, the densities and temperatures of the two knots are the same
within the errors.

\section{NGC~7662}

This bright nebula (PN G106.5-17.6) consist of a
central cavity surrounded by three concentric shells, the inner Rim,
the outer shell \citep{gjc2004}, and a halo \citep{corradi04}.  In addition, on
smaller scales it has a number of LIS. Most of them appear, in
projection, distributed at the outer edge of the outer shell.  All
these structures are easily identified in Figure~\ref{i_ngc7662}, and
are named as in \citet{bea1998} and
\citet{pea2004}. This figure also identify the structures that we
analyze in this paper. \citet{bpi1987} studied the kinematics of the
different nebular components, from which the acronyms FLIERs and
SLOWERs were later introduced.

\begin{figure}
 \begin{center}
 \psfig{file=drg_fig5_a.eps,width=7.0truecm}
 \psfig{file=drg_fig5_b.eps,width=7.0truecm}
 \end{center}
 \caption{NGC~7662: HST archive images. {\it Top}: [O {\sc iii}]. {\it Bottom}: [N {\sc ii}]. In both images the
 box corresponds to 34$\times$34~arcsec$^2$.
 The size of the extraction windows in the spectra are as follows.
  {\it P.A.=175$^{\circ}$ (inner rim + outer FLIER)}: -14\farcs7 to -10\farcs5, SE outer shell;
                                                 -8\farcs4 to -2\farcs8, SE inner rim;
                                                 -1\farcs75 to +1\farcs75, Cavity + Star;
                                                 +2\farcs8 to +8\farcs4, NW inner rim;
						+12\farcs6 to +14\farcs7, NW outer shell.
  {\it  P.A.=248$^{\circ}$ (inner rim + outer shell)}:  -14\farcs7 to -11\farcs2, SW FLIER;
                                                 -9\farcs8 to -2\farcs8, SW inner rim;
                                                 -2\farcs1 to +2\farcs1, Cavity + Star;
                                                 +3\farcs5 to +9\farcs8, NE inner rim;
						+10\farcs5 to +15\farcs4, NE FLIERS. }
\label{i_ngc7662}
\end{figure}

\citet{pea2004} studied this PN with unprecedented spatial resolution
using the STIS spectrograph on the HST. However, their spectra were taken
through two slits (called POS1 and POS2, see their Figure~1), that in terms
of LIS, are restricted to
only one side of the nebula. We have used much longer slits that cover all
the structures along both sides of the nebula, in each direction at P.A.
175$^{\circ}$ and 248$^{\circ}$. This allows us to compare the densities
and temperatures of any given symmetrical
pair of LIS. The slit at P.A. 248$^{\circ}$ contains a pair of
low-ionization filaments (the serpentine-like filaments described in
\citealt{bea1998}). The slit at P.A. 175$^{\circ}$ does not contain any LIS, and is
used to compare the physical parameters along the line joining the
FLIERs with those in a direction free of micro structures. In this
way, the present work can be seen as complementary to the analysis of
\citet{pea2004}.

In Table~5
we report the derived values of $c_{\rm H\beta}$\, that are based on the
average weighted $c_{\rm H\beta}$\ given by the H$\alpha$, H$\gamma$, and H$\delta$\ to H$\beta$\ ratios.
These values are all between 0.13 and 0.21 for the 5 regions under analysis in
each position angle. These $c_{\rm H\beta}$\ agree very well with those previously published:
0.18 - 0.22 \citep{tea1992}; 0.1 \citep{ha1997}; 0.2 \citep{pea2004};
and 0.18 \citet{zea2004}.

This table
gives the observed line fluxes, densities and temperatures of the
10 structures we measured along P.A. 175$^{\circ}$ and 248$^{\circ}$. These
parameters are also presented in Figure~\ref{td_mosaic}.
The average T$_e$[O {\sc iii}]\ derived from the
emission integrated along both P.A. are the same within errors
(T$_e$[O {\sc iii}]=14
300$\pm$700~K and 13 400$\pm$680~K, respectively).  In fact these
values also agree with the T$_e$[N {\sc ii}]=12 750$\pm$1 530~K derived along
the P.A.=248$^{\circ}$.
The T$_e$[O {\sc iii}]\ we obtained here are more in agreement with the
results by \citet{b1986} -- whose [O {\sc iii}]\ temperatures in different
regions of the nebula (see his Table~3) varies from 11 200~K to 13
800~K -- and \citet{zea2004} (13~300~K), than with the somewhat lower
values of \citet{pea2004}.

As for the [S {\sc ii}]\ and [Cl {\sc iii}]\ densities of the integrated emission we
found 2~300$\pm$440~cm$^{-3}$ and 2~550$\pm$490~cm$^{-3}$ for
P.A.=175$^{\circ}$ and 2~850$\pm$450~cm$^{-3}$ and
2~850$\pm$460~cm$^{-3}$ for P.A.=248$^{\circ}$. N$_e$[S {\sc ii}]\ results very
closely reproduce those found by a
\citet[][N$_e$[S {\sc ii}]=2\,884~cm$^{-3}$]{wea2004}.  The same authors give a
value of 1~862~cm$^{-3}$ for the [Cl {\sc iii}]\ density, but errors are not
reported in their work.

Focusing on the densities and temperatures of the inner Rim and
outer shell with respect to those of the FLIERs
(pair of filaments at P.A.=248$^{\circ}$), it is clear from
Figure~\ref{td_mosaic}, that: i) temperatures T$_e$[O {\sc iii}] (where
errors are smaller) are slightly higher at the inner
Rim than in the outer knots (P.A.=175$^{\circ}$), but this is
just at the 2-$\sigma$ level of the adopted errors; ii) densities of the Rim
agree very well one to another in both position angles; iii) the Rim is
roughly a factor of 2.8 denser than the outer shell
(P.A.=175$^{\circ}$); iv) the Rim (inner shell) along P.A.=248$^{\circ}$,
is a factor of $\sim$~1.7 denser than its outer region and the pair
of FLIERs.

Summarising, \citet{pea2004} previously observed the LIS (FLIERs and SLOWERS)
of this PN at different directions than in the present work. Densities for the
FLIERs in both works are in good agreement: N$_e$=2 200~cm$^{-3}$ for the two
FLIERs studied by \citet{pea2004}, and 2 100~cm$^{-3}$ in our work. \citet{pea2004}
did find significantly different densities for FLIERs and SLOWERs, being the
latter approximately 1.3 times denser than the former.

Our analysis shows that FLIERS of NGC~7662\ are less dense than the inner regions
of the nebula, but they are at the same time much denser than the PN outer shell
in which they are located.

\begin{table*}
\centering
\begin{minipage}{120mm}
{\scriptsize
\caption{NGC 7662 Observed line fluxes, flux errors, $c_{\rm H\beta}$, N$_e$\ and T$_e$.
P.A.=175$^{\circ}$ (Rim and Outer shell) and P.A.=248$^{\circ}$ (Rim + FLIERs)}
\begin{tabular}{llcccccc}
\hline
\hline
P.A.=175$^{\circ}$ &  Line ID    & SE outer Shell  & SE inner Rim & Cavity + Star & NW inner Rim & NW outer Shell & NEB\\
\hline
&\multicolumn{7}{l}{}\\
&H$\delta$ 4101.8       &  30.81 &  27.31 &  28.38 & 29.48 &  24.25 & 28.99 \\
&H$\gamma$ 4340.5       &  23.79 &  23.99 &  22.00 & 23.99 &  24.60 & 23.99 \\
&{}[O{\sc iii}] 4363.2  &  17.17 &  15.66 &  19.78 & 18.46 &  19.12 & 17.82 \\
&H$\beta$ 4861.3        &  100.0 &  100.0 &  100.0 & 100.0 &  100.0 & 100.0 \\
&{}[O{\sc iii}] 4958.9  &  504.4 &  368.0 &  343.2 & 338.7 &  481.7 & 372.1 \\
&{}[O{\sc iii}] 5006.86 &  1533. &  1105. &  1018. & 1018. &  1434. & 1114. \\
&{}[CL{\sc iii}] 5517.7 &  0.761 &  0.317 &  1.756 & 0.345 &  0.398 & 0.424 \\
&{}[CL{\sc iii}] 5537.9 &  0.652 &  0.344 &  1.669 & 0.378 &  0.475 & 0.423 \\
&{}[N{\sc ii}] 5754.6   &  0.169 &  0.087 &  0.469 & 0.099 &  0.152 & -     \\
&H$\alpha$ 6562.8       &  331.5 &  324.9 &  334.9 & 326.7 &  334.9 & 339.9 \\
&{}[N{\sc ii}] 6583.4   &  7.496 &  2.981 &  2.502 & 2.540 &  5.191 & 3.115 \\
&{}[S{\sc ii}] 6716.5   &  1.164 &  0.366 &  0.242 & 0.249 &  0.916 & 0.371 \\
&{}[S{\sc ii}] 6730.8   &  1.428 &  0.593 &  0.373 & 0.396 &  1.107 & 0.536 \\
\\
&F$_{{\rm H}\beta}$$^a$ & 3.164          & 36.90          & 14.15          & 30.94          & 2.138          & 104.4 \\
&c$_{{\rm H}\beta}$     & 0.18$\pm$0.017 & 0.16$\pm$0.012 & 0.20$\pm$0.016 & 0.17$\pm$0.015 & 0.18$\pm$0.017 & 0.21$\pm$0.02\\
\\
& & \multicolumn{6}{c}{Percentage errors in line fluxes} \\
\\
&(0.01--0.05)H$\beta$\ &35  &15.5 &12.5 &16.5 &30  &8.5 \\
&(0.05--0.15)H$\beta$\ &16  &10.5 &10   &9.5  &11  &4.5 \\
&(0.15--0.30)H$\beta$\ &10  &8.5  &9    &8.5  &9   &4   \\
&(0.30--2.0)H$\beta$\  &7   &5.5  &7.5  &6	 &7   &3.5 \\
&(2.0--5.0)H$\beta$\   &5.5 &4.5  &5    &5.5  &5.5 &3.5 \\
&(5.0--10.0)H$\beta$\  &5   &4    &4.5  &5	 &5   &3.5 \\
&$>$ 10H$\beta$\       &4.5 &4    &4    &4.5  &5   &3.5 \\
& & \multicolumn{6}{c}{Electronic Densities (cm$^{-3}$) and Temperatures (K)} \\
\\
&N$_e$[S {\sc ii}]   & 1300$\pm$735   & 3650$\pm$1060  & 2950$\pm$730   & 3400$\pm$1050  & 1200$\pm$560	& 2300$\pm$440  \\
&N$_e$[Cl {\sc iii}] & 1250$\pm$700   & 3450$\pm$1000  & 2100$\pm$370   & 3550$\pm$1100  & 1100$\pm$550	& 2550$\pm$490  \\
&T$_e$[O {\sc iii}]  & 12400$\pm$1350 & 13450$\pm$1220 & 15600$\pm$1500 & 15000$\pm$1390 & 13200$\pm$1300 & 14300$\pm$700 \\
&T$_e$[N {\sc ii}]   & 12650$\pm$4830 & 13900$\pm$3350 & -	      & 16850$\pm$4250 & 14450$\pm$5300 & -		\\
\\
\hline
P.A.=248$^{\circ}$ & Line ID   & SW outer   & SW inner & Cavity + Star & NE inner  & NE outer & NEB \\
                   &           & FLIER      & Rim      &               & Rim       & FLIER    &   \\
\hline
\multicolumn{7}{l}{}\\
&{}[S{\sc ii}] 4068.6   & 1.420 & 0.885 & 0.814 & 0.920 & 1.263 & 1.232 \\
&{}[S{\sc ii}] 4076.4   & 0.530 & 0.469 & 0.966 & 0.430 & 0.317 & 0.259 \\
&{}[S{\sc ii}] 4072.0   & 1.923 & 0.954 & 2.127 & 1.131 & 1.381 & 1.804 \\
&H$\delta$ 4101.8       & 24.39 & 24.98 & 25.08 & 23.69 & 23.93 & 23.99 \\
&H$\gamma$ 4340.5       & 43.96 & 45.22 & 45.07 & 44.17 & 43.99 & 45.29 \\
&{}[O{\sc iii}] 4363.2  & 21.83 & 17.27 & 16.43 & 16.53 & 18.89 & 16.98 \\
&H$\beta$ 4861.3        & 100.0 & 100.0 & 100.0 & 100.0 & 100.0 & 100.0 \\
&{}[O{\sc iii}] 4958.9  & 552.7 & 387.6 & 339.8 & 398.1 & 517.8 & 397.1 \\
&{}[O{\sc iii}] 5006.86 & 1706. & 1184. & 1040. & 1214. & 1570. & 1213. \\
&{}[CL{\sc iii}] 5517.7 & 0.637 & 0.395 & 0.408 & 0.389 & 0.606 & 0.410 \\
&{}[CL{\sc iii}] 5537.9 & 0.585 & 0.431 & 0.390 & 0.437 & 0.570 & 0.422 \\
&{}[N{\sc ii}] 5754.6   & 0.585 & 0.088 & -	& 0.089 & 0.552 & 0.155 \\
&H$\alpha$ 6562.8       & 343.8 & 331.9 & 321.6 & 331.3 & 333.8 & 321.1 \\
&{}[N{\sc ii}] 6583.4   & 31.14 & 3.551 & 2.734 & 4.289 & 22.88 & 6.321 \\
&{}[S{\sc ii}] 6716.5   & 2.630 & 0.454 & 0.311 & 0.431 & 2.141 & 0.611 \\
&{}[S{\sc ii}] 6730.8   & 3.843 & 0.751 & 0.423 & 0.679 & 3.064 & 0.932 \\
\\
&F$_{{\rm H}\beta}$$^a$ & 3.580          & 33.59          & 22.23          & 41.22          & 8.732          & 117.9\\
&c$_{{\rm H}\beta}$     & 0.21$\pm$0.025 & 0.17$\pm$0.011 & 0.14$\pm$0.011 & 0.17$\pm$0.011 & 0.19$\pm$0.015 & 0.14$\pm$0.008\\
\\
&  & \multicolumn{6}{c}{Percentage errors in line fluxes} \\
\\
&(0.01--0.05)H$\beta$\  & 38.5 &10.5 &   18 & 9.5 & 25.5 & 8.5 \\
&(0.05--0.15)H$\beta$\  & 19.5 & 8.5 &  9.5 &   7 &   14 & 5.5 \\
&(0.15--0.30)H$\beta$\  &   13 & 6.5 &  7.0 & 5.5 &    8 & 4.5 \\
&(0.30--2.0)H$\beta$\   &  8.5 & 4.5 &  5.0 & 4.5 &    6 & 3.5 \\
&(2.0--5.0)H$\beta$\    &  6.5 & 4.0 &  4.5 & 4.0 &  4.5 & 3.0 \\
&(5.0--10.0)H$\beta$\   &  5.0 & 3.5 &  4.0 & 3.5 &    4 & 3.0 \\
&$>$ 10H$\beta$\        &  4.5 & 3.5 &  3.5 & 3.5 &    4 & 3.0 \\
&  & \multicolumn{6}{c}{Electronic Densities (cm$^{-3}$) and Temperatures (K)} \\
\\
&N$_e$[S {\sc ii}]   & 2400$\pm$1300  & 3950$\pm$650   & 1850$\pm$550   & 3250$\pm$550   & 2250$\pm$800	& 2850$\pm$450   \\
&N$_e$[Cl {\sc iii}] & 1800$\pm$1040  & 3500$\pm$580   & 2150$\pm$630   & 3800$\pm$1370  & 2000$\pm$790	& 2850$\pm$460   \\
&T$_e$[O {\sc iii}]  & 14750$\pm$1980 & 13650$\pm$970  & 14100$\pm$1070 & 13300$\pm$820  & 12700$\pm$1100 & 13400$\pm$680  \\
&T$_e$[N {\sc ii}]   & 11350$\pm$4540 & 12600$\pm$1920 & -	      & 11700$\pm$3920 & 12900$\pm$3720 & 12750$\pm$1530 \\
\hline
\hline
&\multicolumn{7}{l}{{\bf $^a$} In units of 10$^{-13}$erg cm$^{-2}$ s$^{-1}$. Note that
[N{\sc ii}] 6548\AA\ was not measured for any of the structures. Thus, T$_e$[N {\sc ii}]}\\
&\multicolumn{7}{l}{were calculated assuming the theoretical relation between
[N{\sc ii}] 6583\AA\ and [N{\sc ii}] 6548\AA.}\\
\end{tabular}
}
\end{minipage}
\label{t_n7662}
\end{table*}

\section{Discussion}

\subsection{Temperature of the knots}

We have estimated individual temperatures T$_e$[O {\sc iii}]\ and T$_e$[N {\sc ii}]\ for the different regions
of the four nebulae studied in this paper. As it is well known, temperature errors are
always important and they range in our case typically from around 1000 K for T$_e$[O {\sc iii}]\ in
the brighter zones to more than 4000 K for T$_e$[N {\sc ii}]\ in the fainter regions. Therefore, a
sensible comparison of temperatures for the different components of each PN is precluded,
and only rather general conclusions can be extracted: 1) temperatures are those of normal
photoionized PNe, varying from 9~500 to 14~500~K typically; 2) T$_e$[O {\sc iii}]\ agrees  within
the errors with T$_e$[N {\sc ii}]\ for every PN component measured. 3) No relevant differences between
T$_e$[O {\sc iii}]\ at the LIS and at the higher excitation PN structures are found.

\subsection{Knots density contrasts}

The empirical density contrasts between the knots and the inner nebular regions,
as described in this paper, are such that knots are typically 1 to 3 times {\it less dense}
than the rims or cores of these PNe (He~1-1, IC~2149\ and NGC~7662): in no one of the LIS measured
here the electronic density is definitely larger than at the main PN structures. This
unexpected result is nevertheless also found in the full sample of PN with LIS.
Table~4 of \citet{gcm2001} lists 26 PNe with pairs of knots similar to those in the
present work. We have searched in the literature for density measures both
at the inner rims (or shells) of each PNe and at their pairs of knots, finding
eight\footnote{NGC~4634 \citep{guerrero08}; Hb~4 \citep{hajian1997}; IC~4593
\citep{corradi97}; NGC~7009 \citep{gea2003}; K~3-35 \citep{miranda00}; NGC~6826
\citep{bea1994}; NGC~2440 \citep{cuesta00}; K~1-2 \citep{exter03}.} PNe (in addition
to the four nebulae here studied) with adequate data. In all but one PN (NGC~6826)
the densities of the knots are {\it equal or lower} than those of the inner rims
or shells, by factors between 1 and 10.

\begin{figure*}
\psfig{file=drg_fig6.eps}
\caption{Diagnostic diagrams for spatially resolved PNe.
Left panels are an adaptation of the \citet{raga08} results, whereas right panels superpose to these results the data for our sample.
The \citet{raga08} simulations for high-velocity shocked knots that travel through a photoionized region of a PN involve four families of models, as indicated in the labels of the upper left panel. Coded in their names, the numbers represent the knot's velocity, from 40 to 150 ~\relax \ifmmode {\,\rm km\,s}^{-1}\else \,km\,s$^{-1}$\fi whereas letters from `a' to `C' indicate different stellar luminosities and temperatures which are kept constant in each model while the knot's distance to the ionizing source decreases. Therefore, model `a100' has the lowest, and `C100' the highest, photoionization rate, while both assume a velocity of 100 ~\relax \ifmmode {\,\rm km\,s}^{-1}\else \,km\,s$^{-1}$\fi for the knots.
A compilation of empirical literature data performed by \citet{raga08} is also sketched in the four panels as regions filled with diagonal lines.
In the two right panels, different regions of the PNe of our sample are added: empty symbols correspond to the pairs of knots, filled symbols to the nebular inner regions (Rim, Core, Cavity + Star), and half-filled circles correspond to the outer shells.}
\label{raga}
\end{figure*}

This result is not consistent with the theoretical expectations. The formation of PN major
structures and pairs of jets/knots has been modeled in the past using a broad variety of
processes and scenarios (see, for instance, \citet{gcm2001} and \citet{bf2002}). Recent
models can be grouped into three main families. i) Magnetohydrodynamic disk wind models,
based on the scenario of accretion disks formed by binary interactions
(\citealt{fb2004}, \citealt{blackman2001}). ii) Interacting AGB and post-AGB wind
models, in which the post-AGB wind is driven exclusively by the magnetic pressure of a
single star (Garc\'\i a-Segura, L\'opez \& Franco 2005, \citealt{garcia2008}).
iii) Models that explore the effect of axisymmetrical light (low density) jets that,
for a short period of time, expand into a spherical AGB wind \citep{akashi2008}. Some of
the above models are particularly tailored to reproduce the main morphological and kinematic
properties of a few well observed PNe: He~3-401, M2-9 and He~2-90 \citep{g-segura2005}; Mz~3
and the pre-PN M1-92 \citep{akashi2008}. Nevertheless, and despite the different assumptions
of the different models, all of them are able to account for the formation of PNe with jets.

Model predictions state that, after the eventual shut off of the jets, {\it dense} knots would
form embedded in the outer nebular components. Moreover, both the knots present at the tips of
the existing jets and those left over when jets disappear are predicted to be denser than the
inner PN components by large factors ranging from 10 up to 1000 (typically 10) depending on the
model assumptions.

Therefore, there is a clear disagreement between observed and modeled pairs of knots: the former
are found to be typically 10 times less dense, while the latter are expected to be typically 10
times denser, than the inner rims and shells of their parent PN.

A straightforward possibility to reconcile the empirical and theoretical density contrasts is
keeping in mind that empirical densities, as those measured here, correspond to only the ionized
fraction of the PN gas. Models, on the other hand, usually predict the formation of knots accounting
for its morphology, kinematics and total gas content, but do not detail the ionization status of each
component nor their evolution with time. The strong discrepancy between models and observations found
here (a typical factor of 100) can therefore be explained if 90\% or more of the low-ionization knots'
material is neutral. It is worth mentioning here the case of one prominent cometary globule of the
Helix nebula --which contains the best known low-ionization knots of PNe. The molecular matter (H$_2$ + CO;
\citealt{huggins02}) and the dust content \citep{meaburn92} of this knot amount to $\sim$2$\times$10$^{-5}$M$_\odot$,
whereas \citet{ODell96} estimated that the typical mass of the photoionized gas of a globule in Helix is
$\sim$10$^{-9}$M$_\odot$.

In another well-studied system of knots, NGC~7009, previous modeling by \citet{gecac06} succeeded in reproducing the observed ionization structure and chemical abundances under the assumption that the total gas density of the knots is equal to the one empirically derived from the [S {\sc ii}]\ lines \citep{gea2003}, therefore, not accounting for any neutral matter. This apparently contradicts the present results suggesting that the knots might be mostly neutral. However, the effect of the density assumed for the knots in the modeling by \citet{gecac06} is partly balanced by its geometry, i.e., by its shape and size. As the shape was fixed based on the knots' appearance in the HST images, the size was allowed to vary until it fits the observations (i.e. the optical line ratios and electron density). For that reason \citet{gecac06} were able to reproduce the observations of NGC~7009 without invoking need for neutral matter. It would be very interesting to attempt 3D photoionization modeling as in \citet{gecac06} exploring high density regimes for the knots as suggested in this paper.

\subsection{Main excitation of the pairs of knots}

\citet{raga08} have recently simulated the evolution of high-density (10$^3$~cm$^{-3}$),
high-velocity (100 to 150~\relax \ifmmode {\,\rm km\,s}^{-1}\else \,km\,s$^{-1}$\fi) knots that travel away from a photoionizing source
crossing a uniform lower density (10$^2$~cm$^{-3}$) environment. They explored a range of
initial conditions for the shocked knots (in terms of photoinization rate), and qualitatively
reproduced the emission-line ratios of several FLIERs, rims and shells observed in pre-PNe and
PNe. At the end of the model evolution, 400~yr, the number densities for the knots are
10$^3$ to 10$^4$~cm$^{-3}$, broadly in agreement with measured N$_e$\ of knots in NGC~7009 and IC~4634.
These simulations were indeed intended to reproduce the line ratios of the FLIERs of these two PNe.
No predictions are given for the properties of the other PN components (rims, shells and haloes).
 In Figure~6 we show two of the diagnostic diagrams from \citet{raga08} comparing
empirical and theoretical line ratios for FLIERs, as well as showing a compilation of empirical
data for rims and shells of some PNe.

Fig.~6 shows, first, that most of the inner regions (rims and shells) of the PNe in our
sample occupy the same zone as the rims and shells of other PNe in the literature. Second, the
same is
true for the zone occupied by the pairs of knots
in He~1-1\ and NGC~7662\ (open boxes and circles) with respect to the zones of the FLIERs
sample in \citet{raga08}. Third, knots in the other two nebulae, IC~2149\ and KjPn~8\
(open triangles and stars), are displaced from the empirical zone of FLIERs in \citet{raga08}.
Their locations are consistent with the results of simulations with the highest initial
velocity of the knots (150~\relax \ifmmode {\,\rm km\,s}^{-1}\else \,km\,s$^{-1}$\fi, model A/B/C/150), and indicate that a mixing of shock
and photo ionization is playing a role in the measured emission-line ratios. In fact,
the highly supersonic velocity (radial velocity of 226\relax \ifmmode {\,\rm km\,s}^{-1}\else \,km\,s$^{-1}$\fi; \citealt{lmbr1997}) measured
in KjPn~8\  for the SE knot at P.A.=98$^{\circ}$ could explain this agreement. Expansion
velocities of IC~2149's knots are more moderate ($\sim$ 47\relax \ifmmode {\,\rm km\,s}^{-1}\else \,km\,s$^{-1}$\fi; \citealt{vel2002}).

\citet{raga08} show that models with low photoionization rates yield line ratios typical
of shock-excited knots, whereas in models with higher photoionization rate, photoionized
emission dominates the spectrum of the high-velocity, high-density knots. This strengthen
the idea that it is evolution (PN age; see \citealt{g2004},
\citealt{raga08}; \citealt{vii2009}) and photoionization rate (\citealt{d1997};
\citealt{raga08}), rather than the highly supersonic velocities of the knots, the key
parameters to separate the shock-excited from the photoionized structures in planetary
nebulae.

\section{Conclusions}

We have derived the physical parameters of low-ionization pairs of knots,
and of higher ionization PN main components  for a small sample of nebulae (He~1-1, IC~2149,
KjPn~8\ and NGC~7662). We have shown that electron temperatures at the knots are comparable
to the temperatures of the main nebular components, rims and shells, whereas densities
in the latter structures are significantly higher than in the pairs of knots, by up to
a factor of 2. Typical knots' densities in the studied PNe are 500 to 2~000~cm$^{-3}$.

We have argued that optical line ratios are not appropriate to constrain the total gas density, as they only account for the ionized matter of the knots, whereas none of the available models properly explore the knots ionization fraction, but the total (neutral plus ionized) density structure. A direct comparison of our results, plus compiled literature data, with the theoretical density contrasts expected from model predictions, yields a clear discrepancy that amount, typically, up to a factor of 100. To reconcile models and observations we suggest that an important fraction of the gas at the knots --90\%-- should be neutral.
The results presented here can help in constraining more realistic models for jets and
knots in PNe, by providing empirical physical parameters of the ionized gas.

We have analyzed the location of the knots of our four PNe in diagnostic diagrams studied
by \citet{raga08} concluding that the observed line emission ratios are compatible with
shocked knots traveling in the photoionized outer regions of their host PNe.

\section*{Acknowledgments}
We would like to thank the anonymous referee of this manuscript, for his suggestions.
D.R.G. thanks the Brazilian agency FAPERJ (E-26/110.107/2008) for
its partial support. A.M., and R.L.M.C. acknowledge funding from the Spanish Ministry of
Science AYA2007-66804 grant. This paper makes use of data obtained
at the 2.5~m Isaac Newton Telescope (INT: IDS and IPHAS), operated by the Isaac Newton Group;
and at the 2.5~m Nordic Optical Telescope (NOT: ALFOSC), operated by NOTSA. Both are telescopes
of the European Northern Observatory  on the island of La Palma in the Spanish Observatorio del Roque
de los Muchachos of the Instituto de Astrof\'{i}sica de Canarias. We also use NASA/ESA
Hubble Space Telescope data, obtained at the Space Telescope Science Institute,
which is operated by AURA for NASA under contract NAS5-26555.

redpajama_set_name: RedPajamaArXiv


text:
35 Best Bollywood Movies on YouTube to Watch Free
Powered by Rank Math SEO
YouTube is now one of the most used video streaming platforms in the world. Millions of people watch videos daily. Some watch videos on gadget reviews, automobile reviews, cooking videos, fun videos, movie videos, and several more.
So, talking about movies, YouTube is probably the best free video streaming platform that offers tons of movies to watch.
You can watch Hollywood, Bollywood, regional, animation, short films, and international movies too.
Of course, you cannot watch the newly released movies on YouTube, but you don't have to pay to watch a good film either.
There are so many Bollywood movies to watch on YouTube that sometimes it is hard to search them out.
So, in this blog post, I will share 35 best Bollywood movies on YouTube to watch free this lockdown at home.
Due to lockdown, there are a few newly released Bollywood movies too that have been added on YouTube recently.
This will be going to a long list of movies, so don't skip and follow until the end.
Best Bollywood Movies on YouTube to Watch Free
Saand Ki Aankh
Aiyaary
Gulaal
Phas Gaya Re Obama
Tumbaad
Best Bollywood Suspense-Thriller movies and Web Series to Stream on 2020
40 Best Hindi Movies on Netflix India 2020 to Stream Now
Wake Up Sid
Gangs of Wasseypur I & II
RAW – Romeo Akbar Walter
26 Insanely Best Indian Web Series to watch
Chalk N Duster
Shubh Mangal Zyada Saavdhan
Jolly LLB 2
Paan Singh Tomar
Manorama Six Feet Under
Shubh Mangal Savdhan
Socha Na Tha
Naam Shabana
Ayushmaan Khurranna's 'Dream Girl' is a roller coaster film that depicts the life of a jobless Karamvir Singh in a small town who gets pulled into a friendship call center.
Karamvir, who has an innate talent of impersonating a woman's voice, started working as Pooja in that call center.
Meanwhile, he fell in love with the character of Nushrat Bharucha, who plays the love interest of Karamvir (Ayushmaan), and comes the series of twists.
The film is excellent to watch for fun, and Ayushmann's performance is outstanding and near to perfection. It is the combination of Annu Kapoor, Ayushmann, and their brilliant comic timing that makes 'Dream Girl' an entertaining movie to watch.
2019 Bollywood film 'Gully Boy' was one of the most-watched and loved film of that year. Both Ranveer Singh and Alia Bhatt gave one of the best performances of their career and bagged several awards for 2019.
The story is simple but perfectly executed and connected well with the audience.
The protagonist Murad who hails from a poor family dreams of becoming a rapper. But to fulfil his dream he must fight against the social disadvantages. He struggles to achieve what he dreams for.
I don't think there is anyone who hasn't watched the film. It is also streaming on Amazon Prime Videos.
But those who don't have a subscription on Amazon Prime, they can now watch the movie for free on YouTube.
Vikramaditya Motwane's 'Trapped' is quite a promising film that has been entirely carried on by the terrific performance of Rajkumar Rao.
Rajkumar Rao is one of the most underrated actors of the Bollywood who has continued to excel his graph of performances.
Movies like City Lights, Newton, Bareilly ki Barfi, Shahid and Stree were his best. But 'Trapped' is nothing less than his best.
A story of a young man in Mumbai who lives in a flat in an empty high-rise building where he gets trapped when his main door gets auto locked from the inside.
He struggles to survive for days without food, water and electricity. The movie isn't about survival it is about the fears that a person goes through in utter loneliness without a clue of surviving.
In the end, the movie will leave you with a question in your mind, what would you have been done in Shaurya's situation? How would you survive if you would be 'trapped?'
Yet another one of the best non-commercial movies of Raj Kumar that you must watch is 'Newton.'
Two days ago, I suggested my father to watch Newton on YouTube for free.
A simple, effective and moralistic storytelling of a civil servant Newton, who makes sure that a handful of locals in a Maoist-infested village of India can participate in an election.
His unyielding principles and morals forbid him to let go the democratic rights of 76 tribal voters. In the middle of the jungle, ransacking polling station and chased by the armed forces he proved that every vote is counted.
The movie is not dull to watch as there are several comedy cliché that are cynical by nature.
A movie like Newton is what Bollywood needed that bars the unnecessary showcase of pompous plot and gibberish dialogues.
The film raises questions on the democratic voting process in our country, the lack of education about voting and the negligence attitude of the representative and the authorities.
Watch Newton on YouTube now this lockdown, if you have missed it. You won't regret it.
A beautiful story of three friends and their friendship that gets affected by the religious disparities, politics and riots in Gujrat.
Kai Po Che reminds me of Dil Chanta Hai and 3 Idiots. Three friends who has different goals in their life yet bonded together by their selfless love and friendship.
Kai Po Che is a coming – of -age film that put together dreams, aspirations, education system, seeking excellence and friendship.
This is also the movie where Sushant Singh Raput, Amit Sadh and Rajkumar Rao got their big break in Bollywood. The movie was well-appreciated by the audience and earned good figures as profit.
2019 'Saand Ki Aankh' is a Bollywood biographical movie where Bhumi Pednekar and Taapsee Pannu have played grandmothers Chandro and Prakashi Tomar.
At the age of 60+ they picked up guns not to kill but to win a shooting competition. The film is about gender discrimination and violence that takes place in Haryana.
It is challenging what Tapsee and Bhumi has done in the film, playing old woman.
It was quite a controversial topic during the promotion and interviews that both the actors have to face questions on how it make them feel to play older woman character.
It's a fun and inspirational movie to watch that shows us the reality of deep-rooted issue of patriarchy that is still prevalent in every nook and corner of India.
2017 Bollywood film of Hrithik Roshan and Yami Gautam is a box office successful film that has garnered several accolades and awards.
The movie is a simple revenge-thriller where the blind yet confident Rohan (Hrithik Roshan) meets the blind yet independent Supriya (Yami Gautam) and they fell for each other, gets married.
Soon their happy life gets shattered by the intervention of the villain of the movie. The second half of the movie revolves around how Rohan takes a well- planned revenge of his lose.
What makes this film so worthy of a watch?
It is the engaging storytelling and Hrithik Roshan's convincing performance as a blind person in the film. It has turned a sweet fairy tale love story into a nightmare and furthermore, shifted the climax by giving it a twist.
The next one of the underrated Bollywood movies to watch free on YouTube is Aiyaary.
It is an action-thriller film with an intriguing storyline. Director Neeraj Pandey who has proved his metal in directing good movies like Special 26, Baby and A Wednesday. His 'Aiyaary' may not be that good but a worth watching film.
Colonel Abhay Singh chasing Major Jai Bakshi for allegedly betraying his country but Jai is upto something that can prove his innocence and can take him to the real culprit.
I find all the films of Neeraj Pandey similar. They talk about the military intelligence, an attack or a mission. But they all are fascinating to watch till the end.
'Pinjar' is a National Award-winning movie in 2003 that is heart-wrenching and emotional depicts the horror of partition in India.
Puro (Urmila) is abducted by Rashid (Manoj Bajpayee) amid the partition. Puro struggles to survive through the isolation from her family, finding her religion, name and staying with a stranger.
The movie also shines light on the religion disparity, patriarchy, miseries of the women in the name of religion and how it took a toll on the people on both the sides.
The film is intense, deep-rooted to the social issues that are still prevalent in our society even after years of independence.
It is one of the most underrated and underappreciated Bollywood film that you should watch.
Anurag Kashyap's Gulaal is a political and compelling movie to watch. Gulaal follows a multidimensional narrative, a gray storytelling about revolution, betrayal, and conflicts in the political framework.
Director Anurag Kashyap always brings to the audience a dark satirical themed film that reveals the inner darkness of human behaviour. He leaves no fault in his script and execution.
Gulaal is no different. Kay Kay Menon as Dukey Bana is the best to watch.
Ashutosh Gowariker's 'Panipat' is streaming on Netflix now but you can also watch this historical drama film on YouTube for free.
A detailed drama film that portrays the historical facts about Sadashivrao Bhau, a brave commander in Nanasaheb Peshwa's army who won a victorious battle against Ahmad Shah Abdali in Panipat.
The film didn't get much appreciation from the audience, but I find Arjun Kapoor's performance as the mighty commander Sadashiv Rao Bhau worthy of watching.
Phas Gaya Re Obama is a small budget political satire film with a touch of light humour in the narrative.
The story takes us through the journey of Om Shastri (Rajat Kapoor) who is a recession victim lost his job in USA and comes to India to sell his ancestral property to clear his debts. Later, he is abducted by the goons thinking he is a rich NRI return.
It is an amazing film to watch that will not only make you laugh but also make you see the underline ironic comment on the law and administration of the country.
Do you remember watching 'Paa'?
Vidya Balan and Amitabh Bachchan's brilliant performances has made this film so special and heart-warming to watch.
Not only it got countless awards that year but also the audience loved the 13-year-old Auro (Amitabh Bachchan) the most. A kid who looks physically and functions like a 65-year-old man but mentally he is as jovial and lively like a kid should be.
Paa is a tribute to all those kids who are suffering from this disorder. It is an educational and informative film about Progeria.
The script has a simple yet predictable approach and touches the sentimental angle, civic sense, motherhood love and sacrifices.
The beauty of this film is Auro; his innocence, maturity to understand about his medical condition and his subtle pursuit to meet his father in the film makes us love him.
So, how about watching this wonderful film one more time on YouTube for free.
The other day I suggested my mother to watch Tumbaad on YouTube for free. If you ask me why this movie is worth a watch?
I would say, simply because of its unique mythological horror story and outstanding cinematography that I have never watched in any of the Bollywood films.
The film is a tale of gothic, dark and evil that resides inside all of us represented through two characters Vinayak Rao and a mythological demon Hatsar.
Watching the film will give you an incredible cinematic experience. The setting is grim and mysterious from the opening shot taking the story slowly in an unpredictable intense mood.
The characters won't scare you, but the soundtrack and the setting would. If you haven't yet watched Tumbaad, do give it a try for the best performance of Soham Shah.
Ayan Mukherji's coming-of-age film 'Wake Up Sid' is an eye-pleasing movie to watch. The protagonist young lad Siddharth, an irresponsible college guy who doesn't want to take responsibilities.
Soon after meeting with Aisha, he realizes the importance of life, responsibilities and learn to respect.
A simple predictable storyline, with no complexities in the climax or characters. The movie is well relatable with the audience especially with the young audience.
There are chords of emotions that Sid has touched like the relationship he shares with his parents, friends, found his love in photography and how he started embracing happiness in little moments of life.
Yet another outstanding and intense movie of Anurag Kashyap that became one of the most loved movie, only because of two actors Manoj Bajpayee and Nawazuddin Siddiqui.
This crime film is a flawless masterpiece work of an art that portrays the violent blood-drenched gang war, betrayal, revenge, social evils and conflicts in a small town in eastern India.
The movie is split into two part. The first part focuses on Sardar (Manoj Bajpayee) and his revenge that carries a lot of bloodshed and gun fights. The second part focuses on Sadar's sons get entangled in further disputes with the fellow gangs.
One of his son Faizal Khan (Nawazuddin Siddiqui) takes up the revenge saga and vows to wipe out the gang of Ramadhir.
Both the part of Gangs of Wasseypur are outrageous and insane in delivering dialogues. Dialogues that are worth remembering.
It is probably one of the first and best gangster film in Bollywood.
The controversial 'Kabir Singh' is the remake of Telegu super hit 'Arjun Reddy'. The protagonist Kabir Singh is a flawed character who loves Preethi passionately, but circumstances didn't allow them to be together.
The separation left him devastated and he became an alcoholic with no sense of respect left in his eyes. Although many raised questions on how they can portray a character taming a woman and called slapping is okay when there is love.
My perception is , Kabir Singh is a fiction character and in the film the character is damaged and his hasn't been glorified. Only his terrible condition has been shown.
I never liked John Abraham's performances in his movies, it's too flat literally without any expression. But his RAW- Romeo Akbar Walter is a well-intended film about patriotism.
It is a story of an undercover agent who put his life in risk so that he can pass valuable information to the RAW chief to save his country.
I liked how it ended the story. Though the film has nothing special to offer but when you can watch it online for free then why to miss it.
Yet another one of the most underrated and less talked about film in Bollywood is 'Shahid.'
'Shahid' is a brutally honest film that tells the story of a criminal lawyer, who fights for the victims those are wrongly accused by the law.
Raj Kumar Rao as Shahid is brilliant. He has left no gaps in playing the character. It is flawless.
Definitely, one of the best Bollywood movies to watch free on YouTube.
'Neerja' is a biopic story of a brave flight attendant Neerja Bhanot of Pan Am flight 73 in 1986, when the flight was hijacked by the terrorists, Neerja risks herself to save the passengers.
An emotional, inspiring, and heart-wrenching tale of young Neerja, played brilliantly by Sonam Kapoor.
The narrative of the film Neerja is focuses on the realism that had happened on that grim day. It isn't melodramatic, neither the narrative is consumed by emotions.
There is a gentle touch of happiness shown in the relationship that Neerja and her mother played by Shabana Azmi shared. An innocent moment that Neerja had with three terrified kids on the flight.
A movie that everyone should watch.
Nawazuddin Siddiqui's Thackeray is a political controversial movie on the life of Bal Thackeray, the founder of Shiv Sena.
I don't know how much truth there in the story of Thackeray is that has been shown in the movie but the way actor Nawazuddin has played the role with full dedication is one reason for a big applause.
A few ago, when my mother called me and asked for some movies that she can watch on YouTube for free. I told her to watch 'Chalk N Duster.' A film that I knew my mother would love to watch.
'Chalk N Duster' has a solid storyline about the value of good education but unfortunately the makers failed in the execution.
If you can ignore the faults, I will recommend the parents to watch this beautiful film.
Shubh Mangal Zyada Saavdhan is a 2020 romance comedy drama film that follows the love story of two men, Kartik (Ayushmann) and Aman (Jitendra). The narrative has incorporated laughter, humour, social message and sarcasm to deliver their message to the audience.
When small town father Shankar Tripathi (Gajraj Rao), gets to know about their relationship he couldn't accept that and tries hard to separate them.
The story has a very strong concept, but I felt at certain areas it could have been better. Like I felt the character Kartik is over-dramatic. There are times when you will feel the jokes are unnecessary and out of place.
Still, on a wider perspective it is a well-noted Bollywood movie to watch free on YouTube.
Akshay Kumar keeps doing a great many meaningful films. Jolly LLB 2 is the sequel of Jolly LLB. A courtroom drama film where Akshay Kumar who played a lawyer questions the corrupt judicial system and police administration.
The narrative uses dark humour on Jolly that indirectly pointing on us. Usually in films like Pink, where courtroom drama is a serious and intense business. In this movie, the courtroom drama is satirical.
Like always, it is a pleasure to watch Akshay Kumar doing such films.
Deepak Singh (RajKumar Rao) loses his village shop to debt and for survival he along with his family moved to Mumbai. But reaching Mumbai, they never faced a single happy day. They were only tricked by others.
What makes 'City lights' worthy of a watch? It is the breath-taking acting of Raj Kumar Rao. His expressions and his ability to connect with the audience through his character is a great success.
It is a soulful and heart-rendering film that depicts the story of million such people who come to Mumbai in search of work and ends in doing petty jobs.
Most of the time they even struggle to find a shelter and often get tricked by tricksters.
Paan Singh Tomar is a wonderful film to watch. It is a tale of a young army jawan who discovers during his training that he can run faster than anyone.
He earned his name by winning the steeplechase champion, but his fate and some dreadful circumstances turned him into a dacoit.
The sheer simplicity of this film and Irfan Khan's brilliance in acting has made this film one of the best Bollywood movies ever.
How many you have watched Ram Gopal Varma's 'Satya?'
Satya is a Bollywood epic classic gangster movie of Ram Gopal Verma starring Manoj Bajpayee, Urmila Matondkar, JD Chakravarthy and Saurabh Shukla.
Every dialogue and performances of all the cast were superb to watch. There are several gangster movies in Bollywood that over the years have forgotten. But only a few remain on our heart and mind.
Satya and Vaastav are such two movies of the Hindi cinemas that are the best.
I love everything about the movie Queen, a movie for which Kangana Ranaut got the National Film Award for best actress.
In every way she deserves the highly prestigious award for delivering a fabulous performance.
Rani is shattered and devastated after her fiancé (Raj Kumar Rao) broke the engagement just before the wedding. After days she decided to go on her planned honeymoon to Paris alone.
'Queen' is a journey of self-transformation and self-realization of every woman. The film in every way has embrace womanhood.
The transformation of Rani from being an under-confident and timid lady to a confident and graceful lady is wonderful.
She realizes that she doesn't need a man in her life to seek happiness and there are bigger things in life to achieve.
I probably watched Queen 4-5 times and it's an inspiring one.
Manorama Six Feet Under is a very underrated Bollywood film that hardly anyone has watched. It is a brilliant suspense-thriller movie that is inspired by the 70s' noir classic film of Roman Polanski's Chinatown.
Manorama Six Feet Under is not a conventional film to understand. There are layers of complexities that may have left loose to understand.
But that's the amazing fact about this movie. From the opening scene till the end you have to pay attention to details to connect the dots.
A movie that is based on an unconventional topic, a topic that isn't much talked about.
The movie starts with a talented cast that has successfully managed to keep you entertained with humour and with the intention to educate the mass about erectile dysfunction.
Raj Kumar Rao has never failed to impress the audience with his brilliant performances. In the movie 'Made in China,' the duo RajKumar Rao and Boman Irani were magical to watch.
The plot revolves around a small businessman Raghu Mehta (Rajkumar Rao) who fails in every business idea, but he never gave up.
When he joined hands with a 70 -year-old- sexologist Dr. Vardhi (Boman Irani) his business of making a new product touches the sky.
It is a delightful movie to watch free on YouTube this lockdown.
2005 Imtiaz Ali's romantic drama film 'Socha Na Tha' is an enjoyable light-hearted romance story between Viren (Abhay Deol) and Aditi (Ayesha Takia).
Many of you might not have heard or care to watch this sweet love story film by Imtiaz Ali. You can find this movie streaming free on YouTube.
2006 'Rang De Basanti' is not a typical patriotic movie, it's a thought-provoking story that revolves around five friends. Their lives get completely change after an incident where Ajay (Madhavan) an honest air-force pilot is killed in a plane crash.
The five friends took matters in their hand to fight against the deep-rooted corruption in our country.
Moreover, the movie is still remembered for its foot-tapping music and songs (AR Rehman).
Two years after Baby, comes Tapsee Pannu's Naam Shabana, a kicking performance by Tapsee as Shabana, who is a college goer and lives with her mother.
Her life takes a turning point when her boyfriend was killed by a group of rogues in the road. She was looking for a way to avenge his death.
Meanwhile, she was being watched by Manoj Bajpayee and identified her as a potential candidate for the Indian Intelligence agency.
Tapsee is the hero of this film, she is a strong, determined lady who fights hard. Akshay Kumar did gave an special appearance in the end which was cool.
2012 historical drama film 'Chittagong' is based on the events of British India's Chittagong Uprising.
The movie is set against the backdrop of British Colonial India/ east Bengal where a schoolteacher Surya Sen (Manoj Bajpayee) and his followers are protesting against the British Raj .
While Jhunku, one of his students is narrating the story.
I can't explain why this movie is a trademark of the Hindi cinemas. There will be tons of movies that will get release each year but a film like 'Chittagong' is a masterpiece.
Above are according to me, are some of the best Bollywood movies to watch free on YouTube.
Posted in TV Series & MoviesTagged #bestfreemovies, #Bestmovies, #Bollywoodmovies, Youtube
Previous 10 Best Indian Horror Movies to Watch in 2020
Next 11 Best TVF Web Series to Watch If You Have Missed

redpajama_set_name: RedPajamaCommonCrawl


When using FusionDebug in ColdFusion Builder you may notice problems with the line being highlighted properly when a breakpoint fires or when stepping through a page. This currently occurs in the beta 2 of ColdFusion Builder and the problem has been logged with Adobe.
Note that the current instruction pointer and the stack will show the correct line that the application is on, but this line may not be highlighted. Other lines can also remain highlighted after passing them.


text:
Where does SVB rank all time?
Thread starter ShootingHank
sjm
jay helfert said:
yers
Jimmy Caras belongs on your top five Straight Pool players list. Okay, make it top six.
I think I might go with Nick Varner at six and Jimmy Caras at seven. Almost too close to call.
Fatboy said:
Stu has done a brilliant assessment of the greats and their respective era's in this thread. Mostly I agree with him, if we don't agree it's splitting hairs to which there is no definitive answer. (Old Fatboy stepped up his writing game?) told ya I wasn't that dumb all these years lol j/k. No I didn't hire a ghost writer.
One thing I didn't see mentioned in this thread or I missed it. I'd like to add one thing about SVB, it's not where he ranks. It's about him. We talked in this or another thread about how hard he works. That's not disputable. Plenty of us have seen it first hand.
What I'd like to address is what version of SVB do we have today. I met SVB in Reno June 07-I'm 95% confident at the last Sands Reno tourney which he double dipped Johnny Archer 11-9 11-6 iirc in the finals.
That version of SVB was amazing, but he had rough edges, when he played the first TAR match I bet $15,000 on him playing Cory. Could have bet more, everyone knew Cory and SVB was the "kid" in SD that played good.
I've been lucky enough to be with SVB at 4-5 Mosconi Cups in the practice room, he stayed with me many times in Vegas and I'd spot balls for hours helping him practice-we didn't speak, it was work. Serious biz. I offered to help, he said "thanks". To be a minor minor part and a fly on the wall for his ride to stardom in our little corner of the universe is pretty cool. Front row seats watching him develop into what he is today.
I told this long story to be a show off that my writing has improved and share some lucky moments of my life. SVB and I are friends, we don't talk often but we do talk about pool of course and other things that will never be public(ok fishing duh, who don't know that???)
My final point is this, I believe the current version of SVB is thr best version of SVB I've seen play over the last 14 years. He was a champion in 07. But now he has that polish that comes with experience and hard work. I think he's hitting the CB better than ever, his break 'we already know', his focus and mental toughness has just got better with time.
When does he peak and level off? IDK, he takes care of himself so I expect longer than the players of the 80's. He can still improve a bit from this point I firmly believe.
He will be part of the conversation of the all time greats. For his era he is the man…Kid .
Looking forward to seeing the next 14 years happen. It's been great so far!!
This is how we need to look at pool and respect our players who earn respect. Sure nobody is perfect, but when the fans respect the champions it creates their value. If nobody respected Michael Jordan, he'd be just another player.
just my late night musings
Nicely written, sir.
I'm inclined to agree that Shane remains at the very height of his skills. As we've often noted on the forum, the world has caught up. There are more straight shooters than at any time in our sport's history. Asia has been mass-producing great pool talent for twenty five years now, and in the last decade, the quality of European pool has skyrocketed, and not just at the top, as we recently saw all nine Polish entrants at the World Pool Championships reach Stage 2. Europe's Mosconi Cup team of 2020 had, with Fargo in parentheses, Filler (828) Shaw (824) Gorst (818) Kaci (816) Ouschan (810) for an average Fargo rate of 819, which added up to an 11-3 massacre at the Mosconi.
All the credit to Asia and Europe for stepping up their games, and that's why Shane has to do more than ever before if he is to snap off pool's toughest titles like the World Pool Championship, the US Open 9-ball, and the China Open 9-ball ---- but Shane is still a superstar of the highest order.
Reactions: atlas333, JusticeNJ, Fatboy and 3 others
The_JV
'AZB_Combat Certified'
garczar said:
Why do people keep bringing up pocket sizes??
The entertaining part is that supposedly the "large" pockets at the last World 9 Ball was the reason SVB got knocked out, but in this conversation the large pockets of the older era made it easy for the greats to be great...lol
Pick one people
Reactions: sjm, straightline and Poolmanis
skogstokig
The_JV said:
that's a weird one. the conditions are the same for everyone, and those tables were as you write tighter than most world championships that preceded it. 10 years ago they were buckets in comparison. that doesn't take away from earl's title win in 2002 or mika's the year before. those were brutal fields, pressure was sky high, and even if pockets are tighter now, to me those WPC:s have yet to be surpassed in terms of entertainment value.
alstl
I put him at the top of American players. Look at the international field he took down 5 times in the U S Open.
From 1976 to 1993 it was USA vs USA in the finals. This century there has been a foreign player in every final.
Reactions: something_pool
measureman
alstl said:
Easy fix cancel all visa's.
Reactions: pwd72s and KRJ
"no buds chill"
Yeah, sorry this is confusing to you. If the pockets are easier, then true greatness is less likely to shine through. You have more people playing better because of easier conditions, then it's harder to win every match.
So in this case, you're comparing apples to oranges. People made the argument that you can't judge what you've seen of the old school players because they were playing that well on easier conditions, and you're trying to say that that invalidates a completely different argument that Shane hasn't fared as well under easier conditions because other players can play better than they otherwise would BECAUSE of the easier condtions...
I mean you act as though those two arguments are mutually exclusive when they are actually self supportive...
Reactions: westcoast
jay helfert
Shoot Pool, not people
sjm said:
I'll call it for you. Jimmy Caras! He came out of a ten year retirement to win the U.S. Open Straight Pool at age 57! Jimmy took the game just as seriously and was a lot like Nick; quiet, unassuming and proud. He got tired of people asking him if he could still play with the top players since he was only doing exhibitions. He really showed them, didn't he!
Reactions: atlas333, Mich, bbb and 2 others
ShootingHank
This a horrible era compared to the ESPN days when pool was more mainstream.
I made to make sure to watch these events when they were on.
Better players in the past therefore worthy of ESPN. Now it sucks.
Thx Stu, and again we agree
something_pool
ShootingHank said:
Whether or not pool is on ESPN has nothing to do with how good an era's pros are.
Reactions: Fatboy
hang-the-9
It has nothing at all with how good the players are. No-one outside of the real players can tell the difference. When I play in pool halls with random people around they think I am a pro and I'm barely an A- LOL
I don't think skill of the players has one time been mentioned as to why there is no more pool on ESPN, especially since the idea of players 30 years ago getting better is just an idea, which I don't think is correct at all. I have talked to several top players from the 80s and 90s, Archer and Soquet as some specific ones, they both said the players now are overall better than they were back when they were playing in finals.
BeiberLvr said:
Is there anyway to know what the top 10 or so FargoRates were in the 70s or 80s? Would be interesting to compare to today's top 10.
Accu-Stats has info on the top 10 players using their stat system for pretty much every year/month/event. Also keep in mind "Fargo" the system has not been around back then, but you can certainty see who shot the most with the least errors or won the most tournaments in the Accu-Stats era. In the 70s I think it will be a lot harder to get a solid number though.
Didn't Irving Crane take down a tournament with all the top players when he was in his 60's?
He won in 1972 at age 59.
Crane won almost two dozen major championships, including the World Crown in 1946, 1955, 1966, 1968, 1970 and 1972
Reactions: alstl
ChrisinNC
dr_dave said:
There are also many great female players who were not considered in this list. They probably deserve a separate GOAT list that would include players such as Allison Fisher, Karen Corr, Siming Chen, Jean Balukas, Ruth McGinnis, Ewa Mataya Lawrence, Lori Jon Jones, Robin Dodson, Jeanette Lee, Ga Young Kim, Gerda Hofstatter, Kelly Fisher, Jasmin Ouschan, Vivian Villarreal, Pan Xiaoting, etc. These players are certainly among the GOAT female players, but not the GOAT of all players."
You could have stopped after the first five on that list.
Reactions: dr_dave
hang-the-9 said:
Yea they have accu-stats info.
I remember a friend showing me a young Efren's stats and he was damn near perfect. Of course I didn't how to gauge these numbers but he told me Efren was damn near perfect.
eddieindetroit
Time beats even tall mountains down.
The greatest power pitchers eventually loose a bit off their fast ball. Even Muhammad Ali lost a bit of his crispness. Tyson lost a bit of his power.
Sad but true.
Any athletes longevity is impressive and should be respected.
Reactions: westcoast and Fatboy
ChrisinNC said:
Agreed, but the omission of Han Yu is in error. Han Yu, for my money, is Siming Chen's equal.
He won the 9-Ball division at the Stardust in 1968. He was in his late 50's then.
Reactions: cuesblues, Bob Jewett, alstl and 1 other person


Welcome to Harvey's Remodeling, we provide professional interior home improvement solutions in the Panama City Beach, Florida area. Homeowners and condo owners have counted on us for the past ten years to provide a peace of mind and a positive atmosphere during their interior remodeling experience.
You can count on the same.


text:
Tyson the alpaca takes heavyweight role in search for coronavirus vaccine
Scientists hope nanobodies from the alpaca's blood can form the basis of a treatment for Covid-19. PHOTO: REUTERS
https://str.sg/JPJF
STOCKHOLM (REUTERS) - Scientists in Sweden are hoping an alpaca named Tyson can help deliver a knockout blow in the fight to develop a treatment or vaccine against the novel coronavirus that has killed nearly 400,000 people worldwide.
After immunising Tyson, a 12-year-old alpaca in Germany, with virus proteins, the team at the Karolinska Institute have isolated tiny antibodies - known as nanobodies - from his blood that bind to the same part of the virus as human antibodies and could block the infection.
They hope this can form the basis of a treatment for Covid 19 or eventually a vaccine against it, though the work is at an early stage.
"We know that it is the antibodies that are directed to the same very, very precise part of the virus that are important and that is what we have engineered with this antibody from Tyson," Dr Gerald McInerney, head of the team at Karolinska, said.
"In principle, all the evidence would suggest it will work very well in humans, but it is a very complex system."
Llamas and other members of camel family - as well as sharks - are known to produce nanobodies, which are far smaller than the full-size antibodies produced by humans, and therefore potentially easier for scientists to work with.
A vaccine may still be some way off.
"We will now move forward to going into in-vivo studies, maybe with mice or hamsters or other animals that can be used as a model for Covid 19 disease, but the next step after that we really can't say," Dr McInerney said.
As for Tyson, he has done his job.
Coronavirus microsite: Get latest updates, videos and graphics
Coronavirus explainers: What you should know to protect yourself
Coronavirus visual guide: Interactive graphics on the pandemic
"Tyson is 12 years old, I believe, and he may be looking at retirement soon," Dr McInerney said. "So he'll live out his life on his farm back in Germany."
What you need to know about S'pore's new Covid-19 vaccination strategy
Asia stepping up fight against more infectious Covid-19 variants
Hong Kong cements Covid-19 tests with centres just a 15-minute walk
Covid-19 wave looms in Europe amid vaccine fatigue and false sense of security
askST: What is excess death and what is Covid-19's true toll on the world?
Biden says pandemic is over; survivors and doctors disagree
No plans to include Covid-19 vaccinations in childhood immunisation schedule: Ong Ye Kung
Human development set back 5 years by Covid-19, other crises: UN report


text:
How Andrew Huff Visualizes Writing (Episode 49)
Sarah Hamaker October 5, 2021 0 Christian fiction, romantic suspense, The Romantic Side of Suspense podcast, writing
On this episode of "The Romantic Side of Suspense," I'm chatting with Andrew Huff, author of the action-packed Shepherd Suspense Series from Kregel Publications. The first book in the series, A Cross to Kill, was a finalist in the Mystery/Thriller categories of both the 2020 Foreword INDIE awards as well as the 2020 ACFW Carol Awards. Huff is an accomplished novelist as well as screenwriter and has worked in the church media and entertainment industry after spending 10 years as a leader in local church ministry. He currently calls North Texas home where he and his beautiful wife, Jae, raise their two boys and rescue dog.
"As a younger man, I was really interested in filmmaking," Andy says. "When I'm writing a scene, I may [visualize it as a movie]. In my Shepherd suspense series, there are scenes in each of the books that play out as if I were watching a movie in advance of me writing it. … I take that and start diving into how do I turn this into a written scene."
Listen to the podcast for more from our interview, plus an excerpt from Right Cross.
Connect w/Andrew
Website: https://www.andrewhuffbooks.com
YouTube: https://www.youtube.com/c/AndyHuff
Facebook: https://www.facebook.com/huffwrites
Twitter: https://twitter.com/andrewjohnhuff
Instagram: https://www.instagram.com/andyhuff/
LinkedIn: https://www.linkedin.com/in/andrewjohnhuff/
Download file | Play in new window | Duration: 00:25:15 | Recorded on July 26, 2021


text:
Public Science Literacy Night Friday at Pasadena Elementary School
Published : Friday, March 3, 2017 | 6:36 AM
The Norma Coombs Elementary School (NCES) in Pasadena is holding a Science Literacy Night on Friday, March 3, open for students, parents and members of the community.
The event sponsored by the school and its Parents-Teachers-Students Association will feature a scholastic book fair, science activities and demonstrations, telescopes, taco stands and a Kona ice truck.
Olga Manzanero, Community Assistant at NCES, said the demonstrations will include feature JPL rovers and Caltech scientists, rocket launchers, mentos blasters, astronomy presentations, and many more.
"We have parents that work here and this is a collaboration with some community members, including NASA," Manzanero said. "It's been happening for a few years already under the direction of Dr. Smith. It's the fifth year."
Dr. Smith is Dr. Jennifer Smith Jackson, the Principal at NCES, who has been spearheading the Science Literacy Night since it started.
"She is very supportive. She learns everybody's name by heart," Manzanero said. "She is dynamic. While she's talking to you, she's already thinking about the next event. She is a firm believer that if a student knows how to read, she can excel in every other subject. She invests her time in reading about programs that support literature."
The event is free admission and will run from 6 p.m. to 9 p.m. at the school compound at 2600 Paloma Street in Pasadena.
For more information, call (626) 396-5660 or visit www.docdro.id/ehEJjN3.


Locate Flagstaff, Arizona Long-Term Drug Rehab - Drug Treatment and Alcoholism Treatment Centers.
Long-term drug rehab in Flagstaff is a program which offers rehab for not less than 90, but as long as four to six months in some instances depending on the program of preference. Long-term drug rehabs in Flagstaff, Arizona are the favored option when this option can be chosen, because success rates prove that individuals benefit from the level of rehabilitation and exclusive setting offered in long-term programs. Centers which offer short-term rehab, thirty days or less, are normally only able to help individuals overcome physical hurdles when they first abstain from drugs and alcohol. This is the tip of the iceberg, and individuals who only go so far as to deal with physical symptoms have a similar chance of relapsing as somebody who never made it rehab.
No one should risk this occurring to them, particularly if they made the effort to make it to rehabilitation and want this to be a successful and fruitful venture. The final objective is to maintain the abstinence they attain in rehab, so people should steel themselves for what it will require to do this which won't necessarily be easy or fast. In a long-term drug rehab in Flagstaff, AZ., this generally entails a concerted effort on the part of rehab counselors and willing treatment clients to deal with any concerns in the individual's life which could jeopardize their abstinence as well as their dreams of a drug free and happier future. Important changes in lifestyle will be made and every one of these changes will ensure the person has got the best chance at remaining drug free.


Approx. Length: 6 inches, Set of 6 pieces. Elephant key ring included.
Handcraft from natural materials, slight variations from piece to piece should be expected.
Feel closed to nature with ThongDee's eco-friendly wooden kitchen utensils and serving spoons. A warm and wonderful gift for special occasions such as weddings, birthdays, anniversaries and housewarming parties. Happy cooking and meals with nature inspired handcrafts from ThongDee Store every day!


text:
Check it out, Reel Sounds
Bernard Parmegiani: Bruit Force
June 8, 2014 Pam Jahn
Les jeux des anges
Bernard Parmegiani (1927-2013) was one the most formidable composers to emerge from Pierre Schaeffer's music research group the GRM in the 1960s. Parmegiani's work abounds with a vivacious corporeality. His compositions are extremely animated and dynamic, and the sounds he composes with are especially distinctive for their kinetic physicality and visceral presence. They meld environmental noises and impulses with electronic sounds and enhancements in a way that, as clichéd as it is, can best be described as alchemical. Yes, there is much in the way of transmutation or, to evoke Catholicism, trans-substantiation. A sound event or impulse without discernibly doing so becomes another event or impulse, or becomes redolent of something else, and one starts to question the nature of what one is hearing. One becomes an active listener. It is true acousmatic music. There is also a great sense of humour and a genuine sense of motion in his work. Interestingly, Parmegiani trained to be a mime artist with Jacques Le Coq in the late 1950s.
His album De Natura Sonorum (1975) is the defining musique concrète LP, a masterpiece. Notable for its exquisite timbral richness and dynamic interplay, it is also very percussive and physical. When you hear what sounds like a woodblock being struck it sounds and feels like it's happening six inches away from your head. Although it is part of the musique concrète canon and was composed in 1975 it still radiates a sense of being sui generis and extra tempus.
Parmegiani was also a prolific composer for television and cinema, working notably with the Polish auteur Walerian Borowczyk. In Daniel Bird's short documentary Eyes That Listen, he discusses his soundtracks for Borowczyk's animations: 'It's a type of music which on purpose doesn't exaggerate distance from the sound to the image… what you see and what you hear… is as in real life… when something falls down the chute it falls down… da, da, da…' I think he's underplaying just how unique his sounds actually are.
Parmegiani wasn't the only composer Borowczyk worked with. Indeed, the Polish director was something of a pioneer in using electroacoustic music in animation. In collaboration with animator Jan Lenica, he had already worked with composers like Andrzej Markowski and W?odzimierz Koto&#324ski, both members of the Experimental Studio of Polish Radio. It was after Borowczyk came to France in 1959 that he started working with Parmegiani on a number of films, including the macabre 12-minute animation Les jeux des anges (1964).
Perhaps Parmegiani's most widely heard but little known work is the ident for announcements at one of Paris' major airports, Indicatif – Aéroport Paris-Charles-de-Gaulle. This stunning, glistening micro-composition is full of mystery and magic and excited the ears of travellers for 34 years between 1971 and 2005.
I met Parmegiani once. It was at a London Musician's Collective concert at the Institute of Contemporary Art. He was sat drinking wine with his wife, relaxing before he diffused some of his work through a monster sound system. I'd recently released a 20-minute composition on a 3" CD published by the Spanish label Oozebap. I gingerly approached Parmegiani and offered him a copy of the CD. He asked me what was on it and I said 'It's a collage…' He looked back at me doubtfully and said with a slight rising inflection and hint of incredulity, 'You like collage?' I don't recall my reply.
Camera Obscura: The Walerian Borowczyk Collection is released by Arrow Academy on 8 September 2014. This unique limited edition box set (dual format DVD + Blu-ray) includes the short films, The Theatre of Mr and Mrs Kabal, Goto, l'île d'amour, Blanche, The Beast and Immoral Tales.
Richard Thomas will be part of a musical response to Walerian Borowczyk's film scores at Café Oto, London, on 10 June 2014: Octothorpe presents Borowczyk: Mise-en-scène, featuring Aleks Kolkowski + The Dufay Collective (Vivien Ellis, Jon Banks, Paul Bevan & William Lyons) + Secluded Bronte (The Bohman Brothers & Richard Thomas) + short films.
Listen to Richard Thomas's Bernard Parmegiani obituary/homage programme made shortly after his death.
animationfilm musicfilm scorefilm soundtrackGRMmusique concretePolish cinemaWalerian Borowczyk
Previous PostThe Sacrament: Interview with Ti WestNext PostThe Dance of Reality: Interview with Alejandro Jodorowsky
A Deviant View of Cinema – Features, Essays & Interviews
Alter Ego (61)
Cine Lit (10)
Cinema releases (38)
Colonial Report from the Dominion of Canada (22)
DVD and Blu-ray releases (11)
Film Jukebox (69)
Reel Sounds (45)
Short Cuts (48)
Trailers and Videos (1)
1960s cinema
American independent cinema
American independent film
British cinema
Canadian cinema
Chinese cinema
film soundtrack
German Cinema
horror cinema
Korean cinema