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SC Collegium Brushes Aside Govt's Reservation, Reiterates Justice Joseph's Name For Elevation
New Delhi: The Supreme Court Collegium has brushed aside the reservations of the government over its decision to elevate Uttarakhand Chief Justice K M Joseph to the apex court as a judge and...
14 Killed, 17 Injured As Bus Falls Into Gorge In Uttarakhand
New Tehri, Uttrakhand: Fourteen people were killed and 17 injured when the state-run bus they were travelling in fell into a deep gorge around 15 km from Chamba in Tehri district of Uttarakhand on...
5 Boys Rape 8-Year-Old Girl In Uttarakhand
Dehradun: Five boys allegedly raped an eight-year-old girl in their neighbourhood when her parents were not at home in Sahaspur, the police said today. During questioning by police, the...
Trains To Slow Down While Passing Through Rajaji Tiger Reserve
Rishikesh: Trains along the 18-km Haridwar-Rishikesh-Dehradun rail route that goes through the heart of Rajaji Tiger Reserve (RTR) will have to lower their speed for the safety of wild animals. ...
Prez, PM Intervention Sought To End 'Ganga Warrior's Indefinite Fast
New Delhi: Environmentalists and NGOs have sought intervention of President Ram Nath Kovind, Vice-President M Venkaiah Naidu and Prime Minister Narendra Modi to end indefinite hunger strike of Ganga...
23 Dead, 65 Injured As Utkal Express Derails In Khatauli
Muzaffarnagar: At least 23 people have lost their lives and 65 sustained injuries when 13 bogies of the Utkal Express, which runs on the Puri-Haridwar-Kalinga route, derailed on Saturday evening in...
SAD For Reconstruction Of Historic Gurdwara In Haridwar
Chandigarh/Haridwar: Shiromani Akali Dal president Sukhbir Singh Badal today lent its support to the decision of the Akal Takht for reconstruction of historic Gurdwara Sri Gian Godri Sahib at...
11 May 2017 6:42 AM GMT
Baba Ramdev's Patanjali Amla Juice Fails Lab Test, Taken Off Army Canteen Shelves
New Delhi: The Canteen Stores Department, the retailing entity selling consumer goods to armed forces, has suspended sale of a batch of Patanjali Ayurveda's amla juice after it 'failed' to clear a...
25 April 2017 7:57 AM GMT
Jaitley slips while boarding chopper
Haridwar: Union Finance Minister Arun Jaitley today slipped while boarding a chopper in Padartha area in the district where he had gone to visit Ramdev's Patanjali Herbal Food Park.The Minister 'is...
12 March 2017 1:12 PM GMT
Congress Asks EC To File FIR Against PM Modi For Violating Model Code In Haridwar
New Delhi:The Congress on Monday asked the Election Commission to register an FIR against Prime Minister Narendra Modi and other BJP leaders for alleged model code violation by holding a rally at...
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हरिद्वारः बैंक कर्मचारियों ने मांगों को लेकर की एकदिवसीय हड़ताल
हरिद्वारः बैंकों का नियमित कार्य बाहरी स्रोतों से कराये जाने व अन्य समस्याओं पर बैंक कर्मचारियों में आक्रोश बना हुआ है। अपनी विभिन्न मांगों को लेकर यूनाईटेड फोरम ऑफ बैंक यूनियन से जुड़े बैंक...
28 Feb 2017 7:09 PM GMT
हरिद्वारः बिना अनुमति की गई जनसभा पर निष्पक्ष जांच की मांग की
हरिद्वारः कांग्रेस के प्रदेश अध्यक्ष किशोर उपाध्याय ने प्रेस वार्ता में ऋषिकुल मैदान में पूर्व में आयोजित प्रधानमंत्री नरेन्द्र मोदी की जनसभा की अनुमति न लिये जाने को लेकर कई प्रश्नचिन्ह लगाये। किशोर...


The demo is available to download on the Nintendo eShop now.
WarioWare Gold is the first game in the beloved microgames franchise that we have received in a while- and while there are some who might be a bit miffed that it's coming to the Nintendo 3DS, and not the Switch, it is also hard to deny that the 3DS is an inventive machine that can be used for all sorts of unusual applications- in other words, perfect for WarioWare, eh?
If you need more convincing on how this would work, however, there's good news! A demo for the game is available to download on the Nintendo eShop for the 3DS now. The demo will presumably include a sampling of the hundreds (literally) of microgames the final package is slated to have when it launches; at least one new microgame is also included in the demo, though I'll defer to series veterans to be able to identify how many of the microgames in the demo are returning ones from the previous entries, and how many are all new.
Hopefully, WarioWare Gold does well when it launches on the Nintendo 3DS exclusively, later this month in Europe and Australia, and on August 2 everywhere else.


text:
Q: jQuery Keyup Never Entered I am trying to implement an autocomplete capability on an input form in a project that I am working on. I am attempting to use jQuery to trigger an AJAX call to a servlet, and have added a listener on the input field for keyup. However, it appears that it is never entered. I added console logs also to verify that it was indeed not being entered and checking the console it is also blank.
I've included the html below:
<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 4.0 Transitional//EN">

<TITLE>Fabflix Home</TITLE>

Test

<form action = "/FabflixP4/servlet/Movie">
    Search: <INPUT TYPE="TEXT" NAME="title">
    <input type="submit" id="autoSearch" value="Submit">
</form>

I am new to both jQuery and AJAX and figured there is something I am missing. I've spent a few hours now researching this to no avail. As a side not this is a small project not intended for use and performance is not important. Thank you.
Edit1: Added script type and moved to head, still never being entered.

A: You are listening to the keyup event of the submit button. You should listen to the keyup event of the text input.
$('input[name="title"]').on("keyup", function () {

redpajama_set_name: RedPajamaStackExchange


text:
\section{Introduction}\label{sec:intro}
  It is widely believed that protoplanetary disks dissipate inside-out \citep[c.f.,][]{will11}
  and evolve into planetary systems \citep[e.g.,][]{haya85}. When an inner disk at less than $r\sim$1 AU begins to dissipate,
  thermal emission from the disk significantly decreases at near- (NIR) to mid-infrared (MIR) wavelengths corresponding to
  a blackbody temperature of $\sim$100-1000~K.  As a result, a deficit of flux density at $\sim$10 $\mu$m appears in an object's spectral
  energy distribution (SED).  Such objects were first identified with the $IRAS$ satellite \citep{stro89} and are termed
  `transitional disks (in transition between gas-rich primordial disks and gas-poor debris disks)' \citep{calv05,espa14}.
  Recent high resolution and high dynamic range imaging has directly revealed gaps in the central region of disks
  among roughly two dozen transitional disks at NIR \citep[e.g.,][]{thal10,hash12,maya12,debe13,garu13,quan13}
  and (sub)-millimeter wavelengths \citep[e.g.,][]{piet05,brow09,andr11,will11,fuka13,pere14}.
  Some transitional disks also show asymmetries in their dust continuum \citep[e.g.,][]{brow09,pere14}.
  To explain how the gap and the asymmetry form,
  a number of scenarios have been proposed: disk-planet interaction \citep{papa07,zhu11,dods11},
  photoevaporation\citep{clar01,alex06,alex07}, grain growth \citep{dull05,birn12},
  anticyclonic vortex \citep{rega12}, eccentricity \citep{kley06,atai13},
  and their combinations
  \citep[dust filtration; radiation pressure;][]{rice06,dong12a,zhu12,pini12,owen14}.

  Different gap formation scenarios could result in different radial distributions of the surface density
  of the gas and dust grains.
  For instance, {\it disk-planet interactions} will open a gap in the disk, but will have little effect
  on the inner gas-disk \citep[e.g.,][]{zhu11}. Optically thick inner and outer disks in the optical/NIR wavelengths
  would be separated by an optically thin gap.
  {\it Photoevaporation} should remove almost all the gas at the inner disk quickly, leaving a gas free cavity \citep[e.g.,][]{alex07}.
  A supply of fresh material from the outer disk through mass accretion could be halted by a photoevaporative wind,
  resulting in remaining dust grains in the inner disk rapidly draining onto the star and creating a cavity
  (containing empty or optically thin materials).
  {\it Grain growth} would mainly affect the dust grains, leaving gas unaffected \citep[e.g.,][]{dull05}.
  \citet{birn12} demonstrate that grain growth could account for the deficit of NIR and MIR excess in the SED of
  transitional disks, whereas they predict large (millimeter size) dust grains still remain
  in the inner disk region.
  Another intriguing scenario generating different radial distributions
  could be {\it dust filtration} \citep[e.g.,][]{rice06}, whereby large dust grains are trapped at the gas-pressure-bump,
  while small dust grains mixed well
  with the gas still inflow onto the central star.
  {\it Radiation pressure} from an accreting planet \citep{owen14} can also influence its nearby environment. When a massive planet
  ($\gtrsim$3-4~$M_{\rm Jup}$) opens a gap and has sufficient mass accretion from the outer disk, radiation pressure
  from the planet is expected to hold back small dust grains, allowing the dust-free gas to accrete onto the central star.
  On the other hand, {\it anticyclonic vortices} \citep{rega12} and {\it eccentricities} \citep{kley06}
  result in asymmetric structures in the disk.  Anticyclonic vortices induced at the steep gas-pressure gradient such as a `dead zone' \citep{gamm96} and a gap-edge sculpted by
  planet(s) have a higher gas surface-density and efficiently gather dust particles into central vortices;
  eccentric disks formed by a massive planet create a `traffic jam' of the gas and dust grains at the disk apocenter and
  result in steady asymmetric features.

  Determining the radial and azimuthal
  distributions of these disk components (the gas and the small and large dust grains) are crucial
  to understanding the formation of gaps in these disks as well as the origin of observed asymmetries.
  However, transitional disks with a spatially resolved gap in all three disk components
  are relatively rare: AB~Aur \citep{piet05,hash11,tang12}; RX~J1604.3$-$2130~A \citep{math12,maya12}; SAO~206462
  \citep[e.g.,][]{brow09,lyo11,garu13,pere14}; HD~142527 \citep[e.g.,][]{fuka06,casa13};
  Oph~IRS~48 \citep[e.g.,][Follette et~al. in prep.]{geer07,brow12,vand13,brud14}.

  Here we report the results of the dust continuum at 1.3~mm and $^{12}$CO~(2~$\rightarrow$~1) line emission
  from the pre-transitional protoplanetary disk around PDS~70 obtained with the Submillimeter Array (SMA).
  PDS~70 is a solar-type star with a mass of $\sim$0.8 $M_{\odot}$ at an assumed distance of 140~pc \citep{riau06}.
  The other basic properties of PDS~70 can be found in \citet{hash12}, \citet{dong12b}, and references therein.
    The PDS~70 disk exhibits a large gap
  with a radius of $\sim$65 AU at NIR wavelengths \citep{hash12,dong12b}, which
  enables SMA observations to resolve a large gap in both dust continuum and the CO gas.
    In this paper, we discuss the gap formation scenario and the possible origin of fine structures in the disk
    around PDS~70.

  \section{Observations and Results}\label{sec:obs}

  PDS~70 \citep[14:08:10.125, $-$41:23:52.81;][]{cutr13} was observed with the Submillimeter
  Array in three configurations in late 2012 and early 2013 (see Table~\ref{table:pds70obs}).
  The receivers were tuned to place $^{12}$CO~(2~$\rightarrow$~1) in the
  upper sideband, although the exact tuning varied slightly between the
  tracks. The $^{12}$CO~(2~$\rightarrow$~1) line was observed with a resolution of 0.2~MHz in
  the compact and extended configuration, and a resolution of
  0.4~MHz in the very extended configuration. All tracks were gain
  calibrated with 1427-421 and 1325-430 and bandpass calibrated with
  3C~279.
  The absolute flux scale was set by Titan and has a $\sim$10\%
  uncertainty. The data were calibrated in MIR following standard
  procedures\footnote{http://cfa-www.harvard.edu/\~{}cqi/mircook.html} and
  then combined and imaged in Miriad \citep{saul95}. The continuum data
  were concatenated from all chunks with 3.25 MHz resolution, providing
  $\sim$7.5 GHz of continuum bandwidth. The rms in the synthesized beam in
  the very extended configuration are 0.35~mJy~beam$^{-1}$ and 162.5~mJy~km~s$^{-1}$~beam$^{-1}$
  in the dust continuum and $^{12}$CO~(2~$\rightarrow$~1) line emissions, respectively.

  The dust continuum image at 1.3~mm and the integrated $^{12}$CO~(2~$\rightarrow$~1) line emission map (natural weighting)
  in the very extended configuration as well as the 1.6~$\mu$m polarized intensity image of PDS~70 are shown in
  Fig.~\ref{res:dust_pds70}. The images of the dust continuum and $^{12}$CO~(2~$\rightarrow$~1) emissions in the very extended
  configuration have a peak flux of 13.6~mJy~beam$^{-1}$ and 1.06~Jy~km~s$^{-1}$~beam$^{-1}$, respectively. Meanwhile,
  in the combined images of the compact; extended; very extended configurations, a total flux of the dust continuum and integrated
  line emissions above 3~$\sigma$ has 38.1~$\pm$~1.1~mJy and 3.5~$\pm$~0.4~Jy~km~s$^{-1}$, respectively.
  All three images in Fig.~\ref{res:dust_pds70} show
  a deficit of flux density in the central regions of the disk,
    suggesting a
  central cavity or gap structures in small and large dust grains and the gas.
We note that the NIR image alone does not provide convincing proof for the deficit of dust grains in the central region of the disk \citep{taka14}. \citet{taka14} shows that the such a deficit in the NIR flux still allows the possibility of a disk surface that is parallel to the light path from the star, or a disk that is shadowed by structures in the inner radii.

  The morphological structures in the dust continuum and NIR polarized intensity are asymmetric:
    $1.38 \pm 0.06$ and $1.32 \pm 0.15$ times brighter in the north-west part of the dust continuum and the south-east part of
    NIR polarized intensity, respectively, while the brightness of the CO~(2~$\rightarrow$~1) map exhibits no clear asymmetries
      within the limits of observational errors (i.e., it is
    $1.43 \pm 0.38$ times brighter in the south-east region).
  Note that although the orientation of the disk-major axis in the dust continuum image (Fig.~\ref{res:dust_pds70}a) and
  the NIR polarized intensity image (Fig.~\ref{res:dust_pds70}c) appear different from each other (PA of 135$^{\circ}$ and
  160$^{\circ}$ respectively), this is due to the elongated beam in the SMA observations.

  Fig.~\ref{res:vel} shows channel maps of the $^{12}$CO~(2~$\rightarrow$~1) line emission with the LSR velocity range from
  2.65~km~s$^{-1}$ to 8.48~km~s$^{-1}$.
    Since the $^{12}$CO line could easily turn out to be optically thick, we can estimate the gas temperature
    based on the line intensity. The peak flux in the channel maps is 0.46~Jy~beam$^{-1}$ at 7.42~km~s$^{-1}$ and
    suggests $\sim$28~K with the Rayleigh-Jeans approximation.
  A velocity gradient from the northwest to southeast can be seen in the channel maps (Fig.~\ref{res:vel}),
  suggestive of rotation. This velocity gradient can also be seen in the intensity-weighted mean velocity map
  (Fig.~\ref{res:gas}a). Assuming PDS~70 is surrounded by the Keplerian disk with an inclination of 50$^{\circ}$ \citep{hash12},
  we infer a dynamical mass of the central star with 0.6-0.8~$M_{\odot}$ in the position-velocity diagram (Fig.~\ref{res:gas}b),
  consistent with the value of 0.82~$M_{\odot}$ estimated by the spectral type of K5 \citep{riau06}.
  We also found the peak positions between the dust continuum image and the line-emission map are apparently
  slightly misaligned in Fig.~\ref{res:gas}(c): the northwest parts are roughly aligned,
  while the southeast parts have a misalignment with $\sim$$0\farcs25$ (35~AU).
  However, the peak-position determination accuracy strongly depends on the peak flux-density and the signal-to-noise ratio;
  hence, this misalignment seen in our noisy CO data may not be real.

  \section{Radiative Transfer Modeling}\label{sec:model}

  In our previous studies \citep{hash12,dong12b}, we modeled the SED and NIR polarized intensity of PDS~70
  using a Monte Carlo radiative transfer (MCRT) code \citep{whit13} to derive the morphological structure of the dust disk,
  especially in small dust grains. Whitney's code follows a two-layer disk model with small (up to $\sim$$\mu$m size)
  dust grains in the upper disk-atmosphere and large (up to millimeter size) dust grains in the disk mid-plane \citep[e.g.,][]{dale06}.
  Historically, numerical simulations of a disk containing only small dust grains failed to reproduce millimeter-wave emission
  in typical T~Tauri~stars due to the low opacity of small dust grains at longer wavelengths \citep{dale99},
  whereas a disk with only large dust grains was predicted to have no silicate emission bands \citep{dale01}
  ubiquitously seen in T~Tauri~stars \citep[e.g.,][]{furl09} due to the gray opacity of large dust grains at shorter wavelengths.
  Thus, a two-layer disk model has been employed to improve the agreement with observations
  \citep[e.g.,][]{chia01}.

  In this paper, we attempt to simultaneously derive the disk properties in small and large dust grains
  by fitting the SED, the polarized intensity image at NIR, and the dust-continuum image at 1.3~mm using Whitney's code.
  Since we mainly focus on the radial distributions of small and large dust grains (especially the radius of the gap)
  in the modeling efforts,
  we attempt to derive the gap-radius by comparing radial profiles of synthesized images and observations.
  Note that the gas is not modeled in this paper.

  \subsection{Dust Disk Structure and Dust Property}\label{sec:struct}

  The dust-disk structure assumed in this paper follows that from  \citet{hash12} and \citet{dong12b}.
  We synthesize the SED, the NIR polarized intensity image, and the dust continuum at 1.3~mm utilizing
  an axisymmetric and flared disk model in which the vertical density structure ($\rho$ in cylindrical-polar
  coordinates \{$R$, $z$\}) in both small and large dust grains is assumed to be Gaussian,
  \begin{eqnarray}
     \rho(R,z) = \frac{\Sigma(R)}{\sqrt{2\pi}h} \ {\rm exp}\left[-\frac{1}{2}\left(\frac{z}{h}\right)^{2}\right],
     \label{eq_dens}
  \end{eqnarray}
  where $\Sigma$ is a surface density; $h$ is a scale height varying as a power law with a radius, i.e., $h \propto R^{p}$.
  To reduce the number of parameters and simplify, we assume $p=1.25$\footnote{A scale height is described as
    $h \approx c_{\rm s} \Omega^{-1}$, where $\Omega$ is the rotational angular velocity of $\Omega \propto R^{-1.5}$ in the Kepler
    rotation; $c_{\rm s}$ is the sound speed of $c_{\rm s} \propto T^{0.5}$. If $T \propto R^{-0.5}$, then $h \propto R^{1.25}$.},
  i.e., a mid-plane temperature of $T \propto R^{-0.5}$ as approximately estimated by millimeter observations \citep{beck90}.
  The scale heights of small and large dust grains are generally different,
  because small dust grains are expected to be coupled well
  with the gas and might have a similar scale height of the gas whereas large dust grains de-coupled with the gas
  could be likely to settle in the disk mid-plane due to the stellar gravity.
  A radial surface density structure ($\Sigma$) in dust grains described in the similarity solution for viscous accretion
  disks \citep{lynd74,hart98} is
  \begin{eqnarray}
     \Sigma(R) = \Sigma_{0} \left(\frac{R}{R_{\rm c}}\right)^{-q}{\rm exp}\left[-\left(\frac{R}{R_{\rm c}}\right)^{2-q}\right],
     \label{eq_sig}
  \end{eqnarray}
  where $\Sigma_{0}$ is a normalized surface density determined by a total disk mass ($M_{\rm disk}$); $R_{\rm c}$ is a characteristic radius;
  $q$ is a radial gradient parameter. In Whitney's code, in order to generate a gap structure in a central region of a disk,
  a surface density of a dust disk inside the gap ($R_{\rm gap}$) is uniformly scaled down as follows,
  \begin{eqnarray}
     \Sigma(R) = \delta \ \Sigma_{0} \left(\frac{R}{R_{\rm c}}\right)^{-q}{\rm exp}\left[-\left(\frac{R}{R_{\rm c}}\right)^{2-q}\right],
     \ {\rm at} \ R \lesssim R_{\rm gap},
     \label{eq_sig_d}
  \end{eqnarray}
  where $\delta$ is a constant depletion factor. Note that we assume $q=1$ as derived in the viscous disk model with
  $T \propto R^{-0.5}$ \citep{hart98}. A radial surface density of small and large dust grains used in our fiducial model
  is shown in Fig.~\ref{density}.

  Dust properties used in this paper follow \citet{dong12b}:
  small dust grains from the standard interstellar-medium dust model (a composition of silicates and graphites; a size distribution of
  $n(s) \propto s^{-3.5}$ from $s_{\rm min} =$0.0025~$\mu$m to $s_{\rm max} =$0.2~$\mu$m) in \citet{kim94} and large dust grains
  (a composition of carbons and silicates; a size distribution of $n(s) \propto s^{-3.5}$ from $s_{\rm min} =$0.01~$\mu$m
  to $s_{\rm max} =$1000~$\mu$m) from Model~2 in \citet{wood02}. Opacity ($\kappa$) of small and large dust grains used in
  our modeling efforts is shown in Fig.~\ref{opacity} \citep[see also Fig.~1 in][]{dong12b}.

  \subsection{Results of Modeling Efforts}\label{sec:result}

  We have synthesized the NIR polarimetric image, the SED, and the dust continuum of PDS~70 by varying the total mass of the disk
  ($M_{\rm disk}$; assuming gas-to-dust mass ratio of 100), mass fraction ($f$) of large dust grains in the total mass of dust grains,
  scale height ($h$) at 100~AU, depletion factor ($\delta$), size of a gap in large dust grains ($R_{\rm gap}^{\rm l}$),
  and characteristic radius ($R_{\rm c}$). The size of a gap in small dust grains ($R_{\rm gap}^{\rm s}$)
  is set to 65~AU because NIR imaging
  constrains
  this size \citep{hash12,dong12b}.
  Most parameters
  are similar to those in \citet{hash12} and \citet{dong12b}
  except the depletion factor and the characteristic radius. Since the procedure in synthesizing NIR polarimetric images
  in \citet{hash12} and \citet{dong12b}
    did not subtract a
  `polarized halo \citep[described in \S~2.1 in][]{hash12}', the depletion factor and
  the characteristic radius in our fiducial models are slightly different from our previous studies. To simplify,
  we assume
  the depletion factor and the characteristic radius between small and large dust grains are same. In addition,
  the scale height inside and outside the gap is also the same. The parameters in the fiducial model
  and previous model
  are shown in Table~\ref{param}.

    Fig.~\ref{comparison} shows the difference of synthesized NIR images between the fiducial model and the previous model.
    The SEDs in two models (Fig.~\ref{comparison}d) are consistent,
    whereas the radial profiles along the major axis are slightly different (Fig.~\ref{comparison}e). After modeling,
    we subtracted the polarized halo from two synthesized images using IRAF\footnote{
  IRAF is distributed by the National Optical Astronomy Observatories, which are operated
  by the Association of Universities for Research in Astronomy,
  Inc., under cooperative agreement with the National Science Foundation.}
    as a same manner in \citet{hash12}.
    We also added an offset value of 0.14~mJy~arcsec$^{-2}$ to the synthesized NIR images.
    Since polarized intensity (PI) is calculated as square-root of sum of squares in stokes $Q$ and $U$,
    i.e., $PI = \sqrt{Q^{2} + U^{2}}$, the noise becomes always positive. The value of 0.14~mJy~arcsec$^{-2}$ is the averaged
    noise level in our NIR obsevations. These two operations, subtracting the polarized halo and adding the offset value of
    averaged noise, result in the difference of radial profiles of two models.

  As a result of our MCRT modeling with $9\times10^{8}$ photons, we found the apparent size of the gap is different
  (Fig.~\ref{res:model_pds70}):
  80 and 65~AU in a radius in large and small dust grains, respectively. We also show the dust continuum images with fiducial parameters
  in Table~\ref{param}
  with different sizes
    of a gap in large dust grains ($R_{\rm gap}^{\rm l} =$65, 80, and 95~AU)
  in Fig.~\ref{res:model_pds70}. Dust continuum images are convolved with a 2D elliptical Gaussian function of
  $0\farcs97\times0\farcs48$ at PA~$=$~12.33$^{\circ}$ which is a beam-size in our SMA observations.
  The synthesized dust continuum with a gap-radius of 80~AU (Fig.~\ref{res:model_pds70}b) is
  matched well
  with SMA observations
  except for the asymmetries due to axisymmetric structures assumed in our modeling efforts.
  We compare the averaged radial profile of the
  observed dust continuum with that of synthesized dust continuum (Fig.~\ref{res:model_pds70}d). The radial profiles along
  the apparent major-axis at PA of 135$^{\circ}$ are averaged in the northwest and southeast parts. Though the shapes of the profiles
  are reproduced well
  with the synthesized dust continuum with a gap-radius of 80~AU, the flux density of the synthesized
  dust continuum needs to be multiplied by 1.155 in order to obtain the consistent absolute flux density. This result, that
  the radial profile of the observations is brighter than those of the synthesized dust continuum, implies the flux density
  may be gathered in the northwest rather than azimuthally symmetric.

  The synthesized SEDs in Fig.~\ref{res:model_pds70}(e) do not differ significantly except around 200~$\mu$m.
  Large dust grains in the disk-midplane are heated by the emission from the upper layer of the disk \citep[c.f., Fig.~1 in][]{dale06}.
  Since the temperature of the upper layer of the disk generally decreases with the distance
  from
  a central star,
  the disk-midplane irradiated by the upper layer also cools down with the radius. The different gap-radius in large dust grains
  would reflect the amount of thermal emission around 200~$\mu$m in the SED. The three synthesized NIR polarimetric images are reasonably
  consistent with each other (Fig.~\ref{res:model_pds70}f). Since the opacity at NIR wavelengths
  in small dust grains is $\sim$10 times larger than that in large dust grains (Fig.~\ref{opacity}); and the disk in large dust grains
  is located in the midplane, minor geometric differences of the disk in large dust grains do not affect the NIR scattering image.

    Our modeling efforts in this paper are relatively simple, and the above fiducial model would not be
    the best solution.
      Even so, our disk model with a gap consistently explains the the observed images at NIR and millimeter
      wavelengths and the SEDs. In particular, our modeling suggests different gap radii for small and large grains.
    Further complicated disk models (e.g., not sharp gap-edge) and fitting the visibility profile of the dust continuum
    will be presented elsewhere.

  \section{Discussion}\label{sec:discuss}

  We discuss scenarios to account for the observational features of PDS~70, especially the asymmetries and the different
  gap-radii. Before discussing the possible origin of the complicated disk around PDS~70, we summarize six main observational
  properties of PDS~70.
  \begin{itemize}
  \item[(a)] Infrared to millimeter observations and our modeling suggest that
    the depletion of the gas in the disk as well as large and small dust grains within tens of AU in radius
    (\S~\ref{sec:obs} and \ref{sec:result}).
  \item[(b)] The contrast ratio in the dust continuum of 1.4 (\S~\ref{sec:obs}).
  \item[(c)] The above model suggests
    different gap-radii in small and large dust grains, 65 and 80~AU, respectively (\S~\ref{sec:result}).
  \item[(d)] The existence of the optically thick inner disk of small dust grains at $\sim$0.1~AU \citep{hash12}.
  \item[(e)]
    The upper limit of a planetary mass in the gap is estimated to be $\sim$2~$M_{\rm Jup}$ in our previous studies \citep{hash12}
    based on a hot-start planet model \citep{bara03} and the lack of detection of any point sources in the image.
  \item[(f)] The low mass accretion; PDS~70 is a weak-lined T Tauri star (a H$\alpha$ equivalent width
  of 2.0~\AA; \citealt{greg02})
  \end{itemize}
  Thereby, scenarios proposed to explain both the asymmetries and the different gap-radii of PDS~70 should also explain
  all above observational
  constraints. In this section, we firstly discuss the possible origin of the asymmetries, and then, different gap-sizes independently.
  Finally, we discuss the possible scenario responsible for all observational features and suggest how to
  further constrain
  a proposed scenario in future observations.

  \subsection{Azimuthal Asymmetry}\label{sec:morphology}

  Fig.~\ref{res:dust_pds70} show an asymmetric brightness in the dust continuum at 1.3~mm and NIR polarized intensity.
  Such asymmetries in the dust continuum have been detected in other transitional disks, e.g., LkH$\alpha$~330
  \citep {brow08} and SAO~206462 \citep{brow09}. The contrast ratio of the peak-emission to the opposite-side of the disk is likely to
  be higher among transitional disks around intermediate mass stars (e.g., $\sim$30 in HD~142527; \citealt{casa13,fuka13} and $\sim$130
  in WLY~2-48; \citealt{vand13}) than among solar-mass stars (e.g., $\sim$1.1-1.2 in UX~Tau~A, DoAr~44, and LkCa~15;
  \citealt{andr11}). PDS~70's contrast ratio of 1.4 is similar to 1.3-1.5 in SAO~206462 \citep{brow09,pere14} and slightly higher
  than that among solar-mass stars. The physical interpretation of the asymmetries is still under debate: gravitational interaction
  between
  planet and disk \citep[e.g.,][]{kley12}, large anticyclonic vortex induced by the Rossby wave instability \citep[e.g.,][]{rega12},
  eccentric disk formed by a massive planet \citep[e.g.,][]{kley06}, and an azimuthal variance of temperature and opacity.
  In this sub-section, we discuss the potential origin of asymmetric features observed in PDS~70.

  {\it Disk-planet interaction} --- An embedded
  massive planet with a mass of $\gtrsim$1~$M_{\rm Jup}$ could open a gap and excite a spiral density wave in the disk due to tidal
  interactions, while a less massive planet could only excite a wake
  because the perturbation is not strong enough (see \citealt{papa07}; \citealt{kley12} for a review).
  These interactions could also
  lead to exchange of angular momentum of the gas and dust grains
  in the disk, and are expected to result in asymmetric structures in the disk as well. Actually, previous studies have demonstrated
  the asymmetries in the surface density of the disk using hydrodynamic simulations \citep{dods11,isel13}.
  Though the relationship between disk-planet interaction and asymmetric structures in the disk still remains to be intensively
  investigated, a single massive planet could tend to induce azimuthally symmetric structures except spirals \citep{kley12},
  whereas multiple massive planets could create azimuthal asymmetries \citep{dods11,isel13}.
  Hence, the existence of multiple planets would be one of the key points to explain the observed asymmetries in PDS~70.
  The possible existence of (unseen) multiple planets opening the gap around PDS~70 has already been argued in \citet{hash12,dong12b}
  and been supported by following two aspects: the large gas-gap
  around PDS~70 with a radius of $\sim$65~AU (Fig.~\ref{res:dust_pds70}c)
  could be explained by only multiple planets \citep{zhu11,dods11}; a gap structure (optically thick inner and outer disks separated
  by an optically thin region) inferred from NIR imaging (Fig.~\ref{res:dust_pds70}c) and the SED
  (Fig.~\ref{res:model_pds70}e) is most like due to disk-planet interaction rather than other inside-out scenarios (grain growth;
  photoevaporation; see \S~\ref{sec:intro}). Furthermore, \citet{hash12} put an upper limit of the planetary mass of only
  $\sim$2~$M_{\rm Jup}$ in the gap based on $L'$ band (3.8~$\mu$m) imaging,
thus being unable to discard the existence
  of unseen massive planets with a mass of $\sim$1~$M_{\rm Jup}$.
  Therefore, though further quantitative comparisons between observations and numerical simulations (e.g., comparisons
  between the observed PDS~70's contrast ratio of 1.4 and simulations) are still necessary, we anticipate the observed asymmetries
  in the disk of PDS~70 might be induced by interactions between unseen multiple planets and the disk.

  {\it Anticyclonic vortex} ---
  Asymmetric structures in a disk can be explained without any planets. In the last decade,
  several transitional disks show asymmetric dust continuum emission
  \citep{piet05,brow09,andr11,pere14} and has been explained with large anticyclonic vortex potentially formed
  by the Rossby wave instability \citep[RWI;][]{love99,rega12}. RWI is excited at steep gas-pressure gradients
  in an overdense region where is
  thought to be an outer edge of the `dead zone' \citep{gamm96}.
  The gas in the disk is generally transported from the outer disk through
  mass accretion, possibly triggered by the magnetorotational instability \citep[MRI;][]{balb91}. MRI becomes active when the ionization
  state of the gas is sufficient, meaning an ionized upper layer of a disk and a less dense outer-disk are prone to induce MRI.
  Conversely, a dense region in
  the disk-midplane would have less effective ionization because of gas self-shielding against ionization radiation, resulting in a
  dead zone where mass accretion by MRI is strongly reduced. As a result, a gas-overdense region is expected to form at the boundaries of
  the dead zone \citep{varn06,terq08}, leading RWI to launch anticyclonic vortices. The radius of the outer edge in the dead zone
  strongly depends on the amount of dust grains \citep{sano00} because degrees of ionization in the gas are suppressed by
  recombination of ions and electrons at grain surfaces. Assuming the minimum-mass solar nebula \citep{haya85}, \citet{sano00} estimated
  the dead zone's outer edge is about 20~AU in radius. Since this radius is also a function of the disk's properties
  \citep[e.g., a vertical magnetic field, density, and a temperature of a disk;][]{okuz11}, anticyclonic vortices might take place at
  a radius of 80~AU in the case of PDS~70. However, this scenario would not explain the gap structure even if it explains
  asymmetric structures;
    hence it is unlikely that an anticyclonic vortex induced at the outer-edge of the dead zone could be the main scenario.

  Steep gas-pressure gradients can also form at the gap-edge sculpted by massive planets \citep{papa07,kley12},
  resulting in anticyclonic vortices \citep[e.g.,][]{li05,lin10,zhu14a,zhu14b}.
  Coriolis force in a vortex effectively leads large dust grains into the central
  vortex \citep[e.g., Fig.~1 in][]{barg95}, resulting in an increase in the surface density of the large dust grains
  by more than a factor of 10-100 for fastest drifting particles \citep{zhu14a,zhu14b}.
    \citet{vand13} modeled the asymmetric structures in the dust continuum around WLY~2-48, which has the large contrast ratio of 130,
    with a vortex-shaped dust trap triggered by a companion.
    Although PDS~70 has a contrast ratio in flux density of only 1.4,
    this value may be due to the convolution of the large beam size ($\sim$1$''$) in our observations. Thus
    this scenario of the vortex
    at the planet-induced gap-edges would be applied to explain not only the large contrast ratio in HD~142527 and WLY~2-48
    with $\sim$30 and $\sim$130, respectively, but also the case of PDS~70.

  {\it Variance of Temperature and Opacity} ---
  When a disk is optically thin, the observed azimuthal flux density $F_{\nu}$ is
  \begin{eqnarray}
    F_{\nu} \approx \kappa_{\nu} \times M_{d} \times B_{\nu}(T_{d}) \times d^{-2},
  \end{eqnarray}
  where $\kappa_{\nu}$ and $T_{d}$ are the opacity and temperature of a disk with a mass of $M_{d}$,
  $B_{\nu}$ is the blackbody intensity, and $d$ is the distance \citep[c.f.,][]{drai06}. Since
  the Rayleigh-Jeans limit ($h\nu \ll kT_{d}$) can be applied at (sub-)millimeter wavelengths \citep{beck90,beck91},
  $F_{\nu}$ is
  \begin{eqnarray}
    F_{\nu} \propto \nu^{2} \times \kappa_{\nu} \times M_{d} \times T_{d}.
    \label{flux}
  \end{eqnarray}
  Hence, assuming the azimuthally-symmetric dust opacity $\kappa_{\nu}$ and mass-distributions of the dust grains, azimuthal
  distributions of the observed flux density depend on disk temperature. As mentioned in \S~\ref{sec:result}, since
  the disk-midplane is heated by the emission from the upper layer of the disk, if the stellar radiation is interrupted by an asymmetric
  inner disk (e.g., a warp; an asymmetric puff-up), a shadow cast from the inner disk might cool down disk temperature in the outer
  disk.
  Disk temperature of large dust grains in the mid-plane around $r=$80~AU of PDS~70
  simulated in our modeling efforts is 23~K, corresponding
  to the azimuthal temperature variance of 16-23~K using the contrast ratio of the flux density in PDS~70 with 1.4.
  Thus, we cannot rule out this scenario based on our observations.
    Though whether this scenario of shadowing can directly affect on (sub-)millimeter radiation and azimuthal redistribution
    in a (closer to) optically thin environment is still ambiguous, monitoring observations would be useful to test
    the shadowing-scenario, because a shadow cast from the inner disk is co-rotating with the inner disk.
  The Keplerian orbital velocity ($\omega$) of the inner disk at 0.1~AU (where is optically thick in Fig.~\ref{density}) is given by
  \begin{eqnarray}
  \omega \approx 27 \left( \frac{M}{0.8~{\rm M}_{\odot}}\right)^{\frac{1}{2}} \left( \frac{r_{{\rm d}}}{0.1~{\rm AU}} \right)^{-\frac{3}{2}} \ {\rm [deg~day^{-1}]},
  \end{eqnarray}
  where $M$ is the mass of the central star and $r_{{\rm d}}$ is the orbital radius of the inner disk. Such rotation could be
  observed within a few months.
  Furthermore, a non-axisymmetric illumination from the central star \citep{taka14}
  possibly causes asymmetric distributions of the disk temperature. Assuming PDS~70 has the rotational velocity of $\sim$10~km~s$^{-1}$
  and a radius of 1.39~$R_{\odot}$ \citep{greg02}, the rotation period is $\sim$50~days. Such a periodic fluctuation
  could be also observable within a few months.

  Note that though above discussions are based on the azimuthally-symmetric dust opacity,
  asymmetrically distributed dust opacity could also affect the flux density. If the dust opacity $\kappa_{\nu}$
  is assumed to have a power-law dependence on frequency, $\kappa_{\nu} \propto \nu^{\beta}$ \citep{beck90,beck91},
  the observed azimuthal flux density in equation~(\ref{flux}) becomes $F_{\nu} \propto \nu^{\alpha}$
  (where $\alpha = \beta + 2$) assuming azimuthally-symmetric disk temperature and mass distributions of the dust grains. A power-law
  index $\beta$ is known to strongly depend on size distributions and maximum sizes of dust grains \citep{drai06}. For instance,
  interstellar medium (ISM) dust mainly consisting of sub-$\mu$m size grains which are less (sub-)millimeter emitters shows
  $\beta \approx 1.7$ \citep[e.g.,][]{li01}, while circumstellar disks consisting of both small and large dust grains show
  $\beta \sim 0$ \citep[e.g.,][]{andr07}. Thus, if grain growth locally takes place in the disk due to, for example, anticyclonic
  vortices, asymmetric dust continuum emission could be observed. The parameter $\beta$ in $\kappa_{\nu}$
  of large dust grains in our modeling is
  $\sim$0.6 (Fig.\ref{opacity}), and $\beta$ changing with $\delta \beta \sim$0.017
  reproduces the contrast ratio of 1.4 of PDS~70 at 1.3~mm.
  When dust grains grow into larger dust grains in the disk, this chage in $\beta$
  would be reasonable. Hence, though we
  cannot exclude this scenario based on our single-wavelength observations, future high-resolution multi-color radio
  interferometric observations with ALMA
  could reveal azimuthal $\beta$ distributions, allowing the investigation of whether dust grains locally evolve in the disk.

  {\it Eccentricity} ---
  Numerical calculations expect that when a massive planet with a stellar-to-planet mass ratio of $q \gtrsim 3$-$5\times10^{-3}$ is
  embedded in the disk, an eccentric disk can form at the gap-edge
  \citep[eccentricity of up to $\sim$0.25;][]{kley06,atai13,rega14}.
  Keplerian orbital velocity at the
  apocenter of the elliptic orbits is slower than at the pericenter, resulting in a possible enhancement of disk materials at the
  apocenter of the disk. This scenario makes a `traffic jam' instead of a dust-trap, suggesting a lower azimuthal contrast than
  that in the vortex. According to \citet{atai13}, the contrast ratio of the disk mass between the apocenter and the pericenter is
  $\sim$1.5 \citep[see Fig.~3 in][]{atai13}. This value is consistent
  with that of PDS~70. However, the necessary
  minimum-planetary-mass to induce an eccentric disk around PDS~70 would be $\sim$2-4~$M_{\rm Jup}$; such planetary-mass objects
  in the gap should be detected in our previous observations \citep[see Fig.~2f in][]{hash12}.
  One of the differences in this scenario compared to the above is
  that the asymmetries in an eccentric disk are fixed at the same position instead of co-moving with planets or
  vortices; hence future follow-up observations could confirm whether an eccentric disk forms around PDS~70.

  \subsection{Different Radial Structures in Dust Grains}\label{sec:structure}

  Our observations and modelling efforts suggest that
  the disk around PDS~70 has different radial structures in large and small dust grains: a gap of $r=$80~AU for large dust
  grains and 65~AU for small dust grains (\S~\ref{sec:result}; Fig.~\ref{res:model_pds70}). In \S~\ref{sec:intro}, we mentioned
  grain growth and photoevaporation as potential scenarios to explain the properties of transitional disks \citep[e.g.,][]{clar01,dull05}.
  As discussed by other authors \citep[e.g.,][]{espa14}, these two scenarios are expected to result in inside-out disk-dispersal.
  Since PDS~70 has an optically thick inner disk at $\sim$0.1~AU (Fig.~\ref{density}; \citealt{hash12}), these two would be less
  dominant in PDS~70. Another possible scenario is disk-planet interaction \citep[e.g.,][]{kley12}.
  However, {\it only} gravitational interaction between the disk and planet might result in similar radial structures in
  three disk components (the gas and the large and small dust grains), i.e., no radial difference; thus
  {\it only} disk-planet interaction would also be less likely in PDS~70.
  Other scenarios mentioned in \S~\ref{sec:intro} (dust filtration and radiation pressure) need planet(s) in the gap.
  In this sub-section, we briefly review and discuss the combinations of scenarios: disk-planet interaction with dust filtration
  and/or radiation pressure.

  Dust filtration \citep{rice06,zhu12,pini12,deju13,owen14} is induced at the outer edge of the gap. Dust filtration has been originally
  suggested to explain apparently contradictory transitional disk properties: a T-Tauri-star-like moderate mass accretion rate
  ($\dot{M} \sim$10$^{-8}$ to 10$^{-9}$~$M_{\odot}$~yr$^{-1}$; \citealt{naji07}) with an optically thin or empty inner hole.
  Since the disk-materials in the inner disk are resupplied from the outer disk through mass accretion, moderate mass accretion and
  an inner hole are apparently inconsistent. To interpret these transitional disk properties,
  theorists make use of a physical consequence that dust particles are trapped at gas-pressure maxima. When a dust particle embeds
  in a gaseous disk where the pressure has a radially negative gradient, since the gas rotates with the sub-Keplerian velocity,
  a dust particle feels a headwind and loses angular momentum. On the other hand, when a gaseous disk's pressure has a radially positive
  gradient, for example, at the outer edge of the gap, since the gas rotates with the super-Keplerian velocity, a dust particle feels
  a tailwind and gains angular momentum. Eventually, dust particles are led into gas-pressure maxima. The gas can still accrete onto the
  central star through the gap \citep{lubo06} even there are multiple planets in the gap \citep{dods11,zhu11}.
  That is how large dust grains are distributed at gas-pressure maxima, whereas moderate mass accretion is still observable.

    \citet{zhu12} demonstrated that though dust filtration with a single or multiple planets affects
    (sub-)millimeter dust particles, which possibly accounts for (sub-)millimeter observations of large
    gapped ($r \gtrsim$20~AU) transitional disks with moderate mass accretion of $\gtrsim$10$^{-8}$ to 10$^{-9}$~$M_{\odot}$~yr$^{-1}$,
    the filtration process hardly affects (sub-)micron sized dust particles since small dust
    grains are generally coupled well with the gas.
    This can nicely explain the missing gaps in NIR scattered light images of some transitional disks \citep{dong12a},
    such as SR~21 \citep{foll13}, SAO~206462 \citep{muto12}, and MWC~758 \citep{grad13}.
  Subsequent studies in dust filtration \citep{pini12} calculated the position of gas pressure maxima depends
  on disk viscosity, the planetary mass, and location (e.g., a gas pressure maximum at 30 and 50~AU when
  1 and 9~$M_{\rm Jup}$ at 20~AU, respectively,
  in Fig.~1 in \citealt{pini12}); \citet{deju13} showed observed radii of the gap in the NIR and sub-millimeter wavelengths could also
  depend on the planetary mass and location (e.g, gap radii in the NIR and sub-millimeter wavelengths are 20 and 30~AU, respectively,
  when a planet with 1~$M_{\rm Jup}$ at 20~AU in Fig.~2 in \citealt{deju13}). The radius of the gap in the NIR wavelengths could reflect
  the scattered position at the outer gap-edge of the disk in small dust grains carved by a planetary perturbation,
  while the radius in the
  (sub)-millimeter wavelength reflects the peak position of the dust surface-density (i.e., gas pressure-maximum which slightly locates
  at the far side; see Fig.~7 in \citealt{deju13}).
  The dependence of the dust-gas coupling on the size of the dust grains leads
  to different gap-radii at different wavelength, as seen in PDS~70.
  Such disk systems have been reported in SAO~206462 \citep{garu13,pere14}, HD~100546 \citep{aven14,pine14},
  and Sz~91 \citep{tsuk14}; thus PDS~70 is not unique.

  As pointed out by \citet{zhu12}, one problem in dust filtration is that it is difficult
  to account for the low NIR excess generally seen in transitional disks.
  In addition to dust filtration, to reduce the NIR excess generated from small dust grains, `a planetary accretion luminosity'
  was proposed by \citet{owen14} in which small dust grains are expected to push back by radiation pressure from an accreting planet,
  resulting in allowing the dust-free gas to accrete onto the central star \citep{owen14}. This scenario would be useful to explain
  the properties of general transitional disks with the reduced NIR excess and moderate mass accretion. However,
  in contrast to general transitional disks, weak-line T~Tauri star PDS~70 should have low mass accretion (a H$\alpha$ equivalent width
  of 2.0~\AA; \citealt{greg02}).

  \subsection{Possible Origin of Complicated Disk-Structures}\label{sec:origin}

  Though we have discussed the possible scenarios to explain the asymmetries in PDS~70, all proposed scenarios
  except eccentricity are hardly excluded based on our single epoch and single wavelength observations with SMA
  (\S~\ref{sec:morphology}).
  On the other hand, we found disk-planet interaction $+$ dust filtration could account for different radial structures
  in small and large grains (\S~\ref{sec:structure}).
  In this sub-section, we discuss whether disk-planet interaction $+$ dust filtration is potentially responsible for
  the complicated structures of the disk around PDS~70.

  Planet(s) in the gap could reduce mass accretion and might explain the low mass accretion of PDS~70.
  Though mass
  accretion onto a planet is not conclusively understood, in general, a more massive planet (e.g., 10~$M_{\rm Jup}$)
  or multiple planets (e.g., 1~$M_{\rm Jup}$) could reduce mass accretion onto the central star.
  Since the existence of such a single 10~$M_{\rm Jup}$ planet was already ruled out in our previous studies \citep{hash12},
  accreting multiple planets remain as a possible scenario.
  If a single planet with $\sim$1~$M_{\rm Jup}$ can be assumed to have sufficient mass accretion onto the planet itself
  and induce dust filtration,
  this planet might be responsible for the large-gapped disk-structure in the dust continuum \citep{pini12}
  and low accretion rate of PDS~70.
  However, a single planet would likely induce a relatively symmetric structure in the disk \citep{kley12} and thus be
  inconsistent with the asymmetries observed in PDS~70. Meanwhile, a single planet with $\sim$1~$M_{\rm Jup}$
  could create the asymmetries in the disk if vortices take place at the gap-edge sculpted by this single planet.
  However, a single planet is expected to create a narrow gap in the gas and small dust grains
  \citep[i.e., $r\lesssim$15~AU;][]{zhu11,dods11};
  hence a single accreting planet inducing vortices would be ruled out as the origin of the large NIR gap around PDS~70.
  Remaining accreting multiple planets could explain both of low mass accretion and the asymmetries of the large gapped-disk in PDS~70.
  These combinations could also induce dust filtration at the gap-edge and are likely to account for
  the different gap-radii in the NIR and millimeter wavelengths.

  To summarize,
  accreting multiple planets inducing dust filtration at the outer gap-edge could explain all observed properties
  of PDS~70: different observed radii of the gap in the different wavelengths; low mass accretion onto the central star;
  a depletion of disk components
  inside the gap except the optically think inner disk; no very massive planets in the gap. However, direct observational evidence
  of dust filtration has not been detected in any disk system. One conclusive observational proof of dust filtration
  would be `a gap in the gas'
  \citep[see, e.g., Fig.~7 in][]{deju13}. As mentioned, in the outside of the planetary orbit, a combination of positive and negative
  gas-pressure gradients is critical to trap large dust grains at gas-pressure maxima. Inside the planetary orbit, gas-pressure would
  have only negative gradients, resulting in the depletion of large dust grains. Future ALMA observations with high-resolution
  and high-sensitivity will enable the detection of a gas gap. Furthermore, detecting any planets in the gap
  would be important to verify whether
  planets form gap structures in the dust grains and induce dust filtration. A hint to enhance the detectability of planets in the
  optical/NIR wavelength may be the planetary accretion luminosity \citep{owen14}. Though a low-mass binary, a companion in the
  gap of HD~142527 (a mass of 2.2~$M_{\odot}$; a distance of 145~pc; an age of 5~Myr; \citealt{verh11}) exhibit
  an accretion luminosity and
  was detected in the narrow band of H$\alpha$ \citep{clos14}. Therefore, integral field spectroscopy combined with angular differential
  imaging \citep[ADI;][]{maro06} or spectral differential image \citep[SDI;][]{raci99} with ADI focusing on accretion-sensitive lines
  such as H$\alpha$ (0.656~$\mu$m); Pa$\beta$ (1.282~$\mu$m); Br$\gamma$ (2.166~$\mu$m); H$_{2}$~$v$$=$$1-0$~S(1) (2.122~$\mu$m)
  may increase the detectability and allow discovery of accreting planets in the gap.

  \section{Conclusion}\label{sec:conclusion}

  We present the dust continuum at 1.3~mm and $^{12}$CO~$J=2\rightarrow1$ line emission of the pre-transitional disk
  around PDS~70 obtained with SMA, and compare these with NIR (1.6~$\mu$m) polarized intensity image from our previous studies
  to investigate the radial distributions of the gas and the large (millimeter size) and small ($\mu$m size) dust grains
  in the disk. The main observational results are as follows.
  \begin{itemize}
  \item Three disk-components (the gas and the large and small dust grains) show the deficit of flux density
    in the central region
    of the disk, suggesting depletion of the materials except small dust grains.
    High-resolution observations using
ALMA would give more stringent constraints on the gas and large dust grains in the inner disk.
  \item
Both large and small dust grains show azimuthal asymmetries.
    The contrast ratio of the flux
    density at the peak position to that at the opposite side is 1.4 in the dust continuum. Since other transitional disks around
    solar-mass stars have the contrast ratio is $\sim$1.1-1.2, the PDS~70's contrast ratio is slightly higher among solar-mass stars.
  \item
    The results of Monte Carlo radiative transfer models suggest different radii
    for the gap edges: 80 and 65~AU for large and small grains, respectively.
  \item We observed a velocity gradient from the northwest to southeast in $^{12}$CO~$J=2\rightarrow1$ line emission, suggesting
    a rotating disk around PDS~70. The position-velocity  diagram of the CO gas infers the dynamical mass of PDS~70 of
    0.6-0.8~$M_{\odot}$, which is consistent with the spectral type of K5.
  \end{itemize}

  We have discussed the possible origin of the azimuthal asymmetries in the disk. Though definite conclusions are not reached from
  our SMA and previous Subaru observations, we anticipate gravitational interaction between multiple planets and the disk, or
  azimuthal temperature and opacity variance, or anticyclonic vortex
  could be responsible for the observed asymmetries.
  Future follow-up observations to test opacity distributions and
  azimuthal rotations of the asymmetries are expected to put further constraints.

  Finally, gap formation with different gap-radii in large and small grains around PDS~70 have also been discussed. As discussed in
  \citet{hash12} and \citet{dong12b},
  both grain growth and photoevaporation are unlikely because they require an inside-out process
  that directly contradicts the presence of optically thick inner disk around PDS~70.
  We argue that
  combinations of accreting multiple planets and dust filtration explain the observations of
  the gap structure, low mass accretion, and different radii in the outer gap-edge as well as
  the asymmetries of PDS~70. Future observations to confirm the existence of multiple planets and dust filtration are desirable.
  In ALMA cycle~2, a spatial resolution will be comparable to 0.$''$1-0.$''$2 of NIR observations.
  Such a higher spatial resolution could resolve local density-enhancement possibly due to anticyclonic vortices at the gap-edge;
  thus our understanding of complicated disk-structures around PDS~70 will be improved in the near future.

  \bigskip

  We are grateful to an anonymous referee for providing
  useful comments leading to an improved paper.
  We appreciate support from the SMA staff.
  This work is partly supported by a Grant-in-Aid for Science Research in
  a Priority Area from MEXT Japan, by the Mitsubishi Foundation,
  and by the U.S. National Science Foundation under Awards No. 1009203 and 1009314.
  This work is partially supported by Grant-in-Aid for JSPS Fellows (No. 25-8826).

redpajama_set_name: RedPajamaArXiv


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In the following study, the researcher considers the Church teaching that the Holy Spirit invokes a desire within the followers of Christ to unite in 'one flock under one shepherd'. The ways that this call to unity has related to the evangelical mission of the Church is also analysed in the light of this statement. The paper begins with a short reflection on the scriptural vision of unity, and some of the historical dilemmas which have damaged that unity. The theological issues which are at the heart of the Ecumenical Movement and the ways that the Magisterium of the Catholic Church has responded to these issues are then briefly addressed. Finally, some of the practical ways that the whole Church can work for unity are discussed.
'stirs up desires and actions in all Christ's disciples in order that all may be peacefully united, as Christ ordained in one flock under one shepherd'(LG 15).
Whilst it is difficult to imagine that all Christians will ever see themselves as being united under one flock, there are many things which they have in common and have the potential to bring them together. For example, there are those who believe in the Trinitarian God, honour the sacred scriptures, and have a devotion to Our Lady. Furthermore, the Catholic Church is working as part of the ecumenical movement to foster good relations with other churches and ecclesiological communities.
Hulmes (2002, p.18) suggests that although it is believed that the ecumenical movement began in the twentieth century, it has a history that reaches back to very beginnings of Christianity. A number of disagreements developed about the mission and nature of Christ as the Gospel spread throughout the Roman Empire. The ecumenical movement could be seen as a reaction to anything that threatened unity amongst the newly baptised. Evidence to support this claim can be found in various scriptural passages. For example, St Paul warned the Corinthians about the dangers of allowing rivalry and jealousy to develop amongst them (1 Cor 3:1-5). There were also problems between Jewish and Gentile Christians regarding circumcision (Acts 15:1-2). Nonetheless, this matter was raised and resolved at the Council of Jerusalem (circa AD 49). In Peter's address in the house of Cornelius, he makes it clear that no distinction is made by Christ between Jew and Gentile, as long as they follow his teachings.Hulmes (2002, p.7) states that the scandal of the division that exists amongst the baptised, weakens the impact Christianity has on the secularised world. Nonetheless, this disaster has been reduced somewhat by the ecumenical movement. He also believes that this intra-faith movement has been established because people have listened to the Word of God, and allowed the Holy Spirit to work through them (ibid). Although Catholic involvement in this initiative was limited before the Second Vatican Council, this changed considerably after the promulgation of, Unitatis Redintegratio, the Decree on Ecumenism, in 1964 (ibid 8). This document reflects a considerable development in the Magisterial thinking about the teachings of the Catholic Church, regarding relationships with other Christian denominations (ibid 9). In other words, the Decree on Ecumenism sets out a framework for meaningful and genuine dialogue between the Catholic Church, and other Christian churches and ecclesial communities. The Magisterium (UR 3) teaches that all people who have been baptised 'are put in some, though imperfect communion with the Catholic Church'. However, the differences that exist between the Church of Rome, and these 'separated brethren' in terms of doctrine, discipline and structure, create considerable difficulties. Nonetheless, the ecumenical movement is working continuously to overcome these obstacles. The Sacred Council not only recognises the baptised brothers and sisters of other denominations, but also hopes that one day they will be restored to full and perfect communion with the Catholic Church, to which 'Our Lord entrusted all the blessings of the New Covenant' (ibid). Furthermore, the faithful throughout the world are urged by the Apostolate to participate in the work of ecumenism. They should strive hard through prayer, word and actions to bring about the 'fullness of unity' amongst Christians which is desired by Christ, and is influenced by the Holy Spirit (UR 4). Nonetheless, interior conversion within the Church, involving a renewal of thinking (Eph 4:23) and of attitudes, is required if ecumenism worthy of the name is to be experienced amongst believers.Bliss (2007, p.77) wrote that: 'there is little doubt that the Orthodox Church and the Catholic Church are one in the essentials', although each has developed certain distinguishing features. Vatican II (UR 15) addresses the relative positions of the Eastern Churches, which have maintained valid sacraments and orders, and the Church of Rome. The Magisterium states that the 'Church of God is built up in stature' when the Churches in the East celebrate the Eucharist. The Sacred Council also highlights a number of other liturgical and traditional similarities which exist between the Catholic Church, and the Churches of the East. For example, Eastern Christians honour the Mother of God in hymns of praise, and give homage to the saints, which include the Fathers of the Universal Church. Catholics are encouraged by the Apostolate to 'avail themselves more often of the spiritual riches of the Eastern Fathers' in contemplative prayer. The Decree on Ecumenism also emphasises the importance of preserving the spiritual heritage of the Eastern Churches, and the hope of reconciliation between Christians in the East and West (ibid). This commitment was renewed when Pope Benedict XVI and the Patriarch Bartholomew I, made a joint declaration in Turkey in November, 2006, to continue to works towards achieving full communion.The Second Vatican Council (UR 19) makes particular reference to the churches, and ecclesial communities which were separated from the Apostolic See during the 16th century Reformation. Amongst these is the Anglican Communion, in which some Catholic traditions and institutions sill exist. The Magisterium recognises the desire for peace between all Christians, and hopes that the ecumenical spirit will increase 'without obstructing the way of divine providence' (UR 24). However, there are 'very weighty differences' between the Catholic Church, and the breakaway churches of the Reformation. Nonetheless, the desire still exists to find ways that allow meaningful ecumenical dialogue to take place. In the conclusion (UR 24) of the Decree on Ecumenism, the Sacred Council acknowledges that achieving unity amongst all Christians is beyond human power, and places its hope in Christ. Nonetheless, the faithful still have an important role to play in bringing about the healing of historical wounds, and working towards reconciliation (Lk 17:3-4).Bliss (2007, p.1) states that 'spiritual ecumenism' or private prayer for Christian unity (UR 8) was an important prelude to the official entry of the Catholic Church into the ecumenical movement at the Second Vatican Council. Nonetheless, Catholic ministers worked along with clergy from other denominations to promote ecumenical initiatives such as the 'World Week of Prayer for Christian Unity' long before the publication of the Decree on Ecumenism. Bliss (ibid) also believes that prayer is the essential element for all those interested in developing Christian unity today. Cardinal Kasper (2007, p.10) said that it was very significant that Jesus did not express his desire for Church unity in a commandment or teaching, but rather in a prayer to his father in Heaven (Jn 17:20-21). The Cardinal (2007, p.11) also said that prayer for unity is the 'royal door of ecumenism' which enables believers to face hurtful memories courageously, whilst deepening the bonds of communion. Nonetheless, spiritual ecumenism also requires a 'change of heart and holiness of life' that is born out of the call of Christ for conversion (ibid). Hulmes (2002, p.38) suggests that the Catholic Church has not always been as enthusiastic about the promotion of ecumenism as she is today, particularly when it involved other world religions. It was extremely difficult to build good relations with men and women of different beliefs through the Church's rigorous application of the extra ecclesiam non est salus (outside the Christian Church there is no salvation) doctrine. Nonetheless, the Second Vatican Council outlined a new approach to inter-faith dialogue in its Declaration on the Relation of the Church to Non-Christian Religions in 1965. The Sacred Council (Nostra Aetate 2) urges the faithful to engage in dialogue, and collaboration with members of other faiths. Furthermore, it 'rejects nothing of what is true and holy' in these religions. Therefore, Christians should: 'acknowledge, preserve and encourage the spiritual and moral truths' which are held by people of different faiths. Nonetheless, they should not make doctrinal or ethical concessions for the sake of developing easier relations with those of other belief systems.
Bliss (2007, p.2) suggests that the Catholic Church has shown a deepening commitment to achieving Christian unity since entering the ecumenical movement. This is demonstrated in the many theological debates which have taken place between the Church of Rome and other churches. A considerable number of magisterial writings have also been issued on the subject of ecumenism. For instance, in 1995 Pope John Paul II (Ut Unum Sint) reiterated the call of the Second Vatican Council for all Christians to unite. He states that 'the unity of all divided humanity is the will of God', this is why Jesus was sacrificed on Calvary (US 5). He also says that love has the power to bring individuals, and communities into perfect communion (US 21). He gives a reminder that when Christians of different traditions gather in common prayer, they invite Christ himself to be with them: 'where two or three meet in my name, I am there among them' (Mt 18:20). In the same year, John Paul II (Orientale Lumen) also said that it was time for the Catholic Church and the Orthodox Church to deepen their level of communion.
In this study, the researcher considers some of the ways that the Church's call to unity has related to its evangelical mission. It seems that there has been a need to work for unity amongst Christians since the early days of the Church. This is evident from the writings of St Paul (1 Cor 3:1-5) where he calls for the Corinthians to abandon the jealousy and rivalry that was developing amongst them. Nonetheless, a considerable number of schisms and disputes have separated Christians over the centuries. The Ecumenical Movement recognises the need for co-operation and dialogue to take place so that the divisions and wounds of the past can be healed. The Catholic Church has not always been enthusiastic about the ecumenical movement. However, it became more committed to working for Christian unity after the promulgation of the Decree on Ecumenism at the Second Vatican Council. This is demonstrated by the large number writings which Catholic bishops have produced on the subject of ecumenism, and the amount of dialogue which they have entered into with other Churches and ecclesial communities since the Scared Council closed. Furthermore, these discussions have reached beyond the boundaries of those of the Christian faith. The Church also realises the importance of fostering good relations with people of different religions. Finally, it is hard to imagine a world that is united in the same belief. Perhaps the way forward is to 'make this pilgrimage together hand-in-hand' as John Paul II suggested at the Mass in Bellahouston Park in 1982.
"Ecumenism." UKEssays.com. 11 2018. All Answers Ltd. 04 2019 <https://www.ukessays.com/essays/religion/ecumenism.php?vref=1>.
"Ecumenism." All Answers Ltd. ukessays.com, November 2018. Web. 24 April 2019. <https://www.ukessays.com/essays/religion/ecumenism.php?vref=1>.
UKEssays. November 2018. Ecumenism. [online]. Available from: https://www.ukessays.com/essays/religion/ecumenism.php?vref=1 [Accessed 24 April 2019].
UKEssays. Ecumenism [Internet]. November 2018. [Accessed 24 April 2019]; Available from: https://www.ukessays.com/essays/religion/ecumenism.php?vref=1.


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Innovation in Advanced Digital Imaging
How 'Hugo' Gave One Neuroscientist the Gift of Stereo-Vision
I'd like to share with my readers an email forwarded to me from Dr. Sue Barry. Dr. Bruce Bridgeman is a fellow neuroscientist who, like Dr. Barry had lived with a type of strabismus commonly called walleyes where the eyes point outward rather than inward. Dr. Bridgeman wrote the email to Dr. Oliver Sacks, one of the most inspiring neuroscientists in contemporary literature. I decided to post this as a follow-up to "People Who Hate 3D Movies Should Get Their Eyes Examined" because Dr. Bridgeman's revelation of stereovision happened while watching Hugo. I believe it was the way Martin Scorsese masterfully pushed the stereo envelope that gave him his first sense of volume and depth in the world. The last sentence in Dr. Bridgman's email summarizing his new found stereo vision once again points to the immense value of immersive 3D in feature films, "I feel myself to be in the visual world, rather than at it."
Email From Dr. Sue Barry
Dear Barry,
Below is the complete text of an email that Dr. Bruce Bridgeman, a professor at UC Santa Cruz, wrote to Oliver Sacks regarding stereovision. As you'll see, Hugo had a profound impact on his vision.
Email From Dr. Bruce Bridgeman to Dr. Oliver Sacks (published with permission from Dr. Bridgeman)
Dear Dr. Sacks,
I'm a neuroscientist who recently had restored stereopsis similar to that of 'Stereo Sue' in 'The Mind's Eye', but with experience rather than professional intervention. My case combined with Stereo Sue's makes me think that therapy for stereo-blindness, perhaps beginning with amplified disparity in natural scenes, should be part of every optometrist's toolkit. I teach the behavioral neuroscience course at UC Santa Cruz; my website below will tell you more than you ever will want to know about my career.
I have had flat fusion since my first corrective lenses at age 21, when my congenital exotropia (walleye) was corrected without prisms. Here is a brief piece about my recent experiences. You can call me 'Binocular Bruce'.
There is a paper on my previous condition:
Schor, C., Bridgeman, B., and Tyler, C.W., Spatial Characteristics of Static and Dynamic Stereo Acuity in Strabismus. Investigative Ophthalmology and Visual Science, 1983, 24, 1572-1579.
Dr. Bruce Bridgeman's Account Of His Experience With Hugo
In Mid-February 2012 I saw the movie 'Hugo' in 3D. Going into the theater my wife and I paid a surcharge for 3D glasses, which I thought were a waste of money for me – having been exotropic since childhood, I was nearly stereo-blind. But I took the polarizing glasses to avoid seeing annoying fringes in the film. To my great surprise, I immediately experienced the film in vivid stereo. I was enthralled. But perhaps the filmmakers exaggerated the stereo disparities in the film to enhance the value of the 3D technology. I still don't know whether that's true. I could find only qualitative estimates of the disparities used in the movie; perhaps the filmmakers thought only in relative terms. Hugo's VFX supervisor Ben Grossmann said "We checked and checked: We were four to six times bigger than any other 3D movie. But everything looked amazing."
I had to concentrate to appreciate the stereo effects, and purposely-blurred objects in the foreground bothered me – they captured my attention even though the filmmakers clearly wanted me to attend elsewhere.
When the movie ended we turned in our polarized glasses and walked out into the street. I was astonished to see a lamppost standing out from the background. Trees, cars, even people were in relief more vivid than I had ever experienced. Clearly the disparities weren't amped up on the street. Did a few hours of enhanced disparity wake up long-neglected binocular neurons in my visual cortex?
There was also an effect on memory; I recall vividly what the street looked liked that night, though I don't particularly recall the appearance of streets after exiting other movies before or since.
In the next few days (after seeing 'Hugo') I began examining the world in a new light. I also enjoyed using binoculars that also magnify disparities, now with 3 modes of vision, left eye, right eye, and stereo; previously I would look through only one side or the other, not needing to close the other eye to suppress the image. Riding to work on my bike I looked into a forest beside the road and saw a riot of depth, every tree standing out from all the others, a 3D feast. At first the best stereo effects were limited to stationary or slowly moving objects, but now a month later I appreciate stereo even as it enhances parallax.
In the ensuing weeks I enjoyed new stereo experiences every day. Trees in the view from our living room previously were just a panel of green, but now were separate objects jumping out at me. On March 7th, a windy day, I saw wind-whipped waves of grass in our back yard. It gave a whole new meaning to 'amber waves of grain'. In dull spots during meetings or talks I can sit back and enjoy the stereopsis.
Entering awe-inspiring European cathedrals I always had to keep moving, sometimes to the annoyance of my companions, to appreciate the dimensionality of the space from parallax alone; I suspect that I could now experience them even better from stereo disparity alone. A year ago Dr. Suzanne McKee gave a masterful talk on stereopsis at our department; I objected that parallax could provide the same information, but she informed me that stereopsis provides finer-grained stereoscopic information than motion parallax, at lower thresholds. That took me aback, as I had thought and taught for years that the two sources of 3D information should be equivalent, one successive and the other simultaneous.
I remember only one stereo experience from my childhood. The back of a cereal box had little cutouts that could be bent forward to stand up when the background cardboard was lying on the kitchen table. Stooping down to put the figures at eye level, I saw them pop out. The disparities must have been enormous, and of course the 3D effect was hyped on the cereal box. I must have been seven or eight at the time. I have had exotropia and alternating strabismus since childhood. At the age of eight I was examined at the Wills Eye Hospital in Philadelphia, where the ophthalmologist recommended against surgery. No treatment was started, but we were poor and may not have been able to afford it. I remained misaligned until I was worked up at the Palo Alto Medical Clinic in 1968, having obtained health insurance as a Stanford graduate student. The optometrist discovered a large horizontal disparity, more than 20 diopters, and a small vertical one. I got my first corrective lenses and did orthoptic exercises such as pencil pushups etc. My eyes became aligned most of the time, but the effect seemed mostly cosmetic.
I have always had the ability to look through either my left or my right eye at will – it's like a saccadic eye movement, except that it's my end of the line of sight that moves rather than the far end. I had the habit of doing near tasks with one eye and far tasks with the other. After getting a spherical correction that gave me good focus simultaneously in both eyes I was able to fuse binocularly if I concentrated and if targets weren't too close, but I got no benefit from it so I didn't do it much.
Something is also lost with stereopsis. Previously I had a vivid perception of juxtaposition of objects, sometimes seeing amusing illusions where one object seemed attached to another. Now each object stands apart, no longer adjacent to more distant objects. But I feel myself to be in the visual world, rather than at it.
Bruce Bridgeman
Research Professor of Psychology
409 Social Sciences 2 Tel. (831) 459 4005
Santa Cruz, Ca. 95064 Fax (831) 459 3519
http://people.ucsc.edu/~bruceb/
I wish to thank Dr. Sue Barry for bringing Dr. Bridgeman's case to my attention and I wish to thank Dr. Bridgeman for permission to publish his letter to Dr. Oliver Sacks.
With over 100 scientific articles in peer-reviewed journals as well as several book chapters Dr. Bruce Bridgeman's research centers on spatial orientation by vision and perception/action interactions. His book, "Psychology and Evolution: The Origins of Mind" (Sage Press, 2003) explores the functions and neural basis of consciousness and the
application of evolutionary theory to psychology. It introduces students to the emerging field of evolutionary psychology. Dr. Bridgeman applies concepts of evolutionary theory to basic psychological functions to derive new insights into the roots of human behavior and how that behavior may be viewed as adaptation to life's significant challenges. Examining courtship, reproduction, child rearing, family relations, social interaction, and language development, Bridgeman uses evolutionary theory to help in the search to elucidate the foundations of human perceptions, experiences, and behaviors.
Posted by Barry B. Sandrew Ph.D. at 7:47 PM
Barry B. Sandrew, Ph.D.
Founder - Graffiti Video, Inc.
This is a series of blogs by Barry Sandrew, Ph.D., an internationally recognized inventor, digital imaging expert and visual effects pioneer. Dr. Sandrew is founder of three visual effects facilities that were among the largest and most prolific production studios in Hollywood. Over the past three decades he has been and continues to be instrumental in evolving the entertainment Industry's digital standards and processes in feature filmmaking.
Sandrew earned his doctorate in neuroscience from SUNY at Stony Brook. After winning a 2 year NIH Fellowship at Columbia University, College of Physicians & Surgeons, he joined Harvard Medical School/MGH as staff Neuroscientist. In 1987, Sandrew left his academic and scientific career to found American Film Technologies (AFT) where he invented the first all digital process for colorizing black and white feature films.
At AFT he also invented a paperless animation process used to produce episodic animation for Fox Children's TV and a digital ink & paint and compositing pipeline that produced Spielberg's first digital animated feature film, "We're Back: A Dinosaur Story." Sandrew took AFT public while converting hundreds of movies for clients such as Turner, Disney, Warner Bros., Fox, Gaumont, TF1, ABC, and CBS, among many others.
In 1993 Barry Sandrew left American Film Technologies to co-found Lightspan, an animation and production edutainment studio that grew into one of the largest educational software companies in the U.S., marketing into entire school districts around the country. Lightspan ultimately went public and was later acquired by Plato Learning.
In 2000, Sandrew founded Legend Films, re-inventing colorization and a proprietary film restoration process using the latest in digital imaging technology. Over the course of the next 7 years, Legend Films converted to color approximately 145 black & white films as well as several TV series. Legend Films also produced visual effects for Scorsese's "The Aviator", HBO's "Entourage" and other high profile TV and film projects.
In 2007, with Jim Cameron's game changing "Avatar 3D" scheduled for a 2009 release, Sandrew leveraged his proprietary colorization pipeline, redirecting his company's entire R&D focus to embrace 2D-to-3D conversion and changing the company's name to Legend3D. Since 2010, Legend3D has lead the competitive field, producing 3D conversion and visual effects on over 35 of the highest performing box office tentpole films of the past 6 years.
In 2014, Dr. Barry Sandrew left Legend3D to focus on new immersive and web based media technologies as well his non-profit and for-profit board positions. He is consultant to Fortune 500 companies re: mobile 3D-sensing and motion tracking technology that he considers precursors to augmented reality. Most recently, he is Co-Founder and President/CEO of Graffiti Video, Inc. a company that is redefining the curation of web based media.
Requests or Calls for:
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Contact Dr. Sandrew -
Email: bsandrew.L3D@gmail.com
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I'd like to share with my readers an email forwarded to me from Dr. Sue Barry. Dr. Bruce Bridgeman is a fellow neuroscientist who, like Dr...
Jared Sandrew, Stereoscopic Supervisor on "The Walk" Discusses His 3D Conversion Of The Sony Blockbuster!
High Tech Props 'The Walk' in 3D Originally published in Examiner by Marlene Sharp , October 2, 2015 The legendary star of ...
Feature Film Critics Who Hate 3D Movies Should Have Their Eyes Examined
This is not intended as an insult, it's a legitimate suggestion because we all experience 3D movies differently, and many of us have visio...
Part 1 - Sitting Too Close To Your 3D TV Will Make You Go Blind?
Well, not really. One of several things my Mom said would make me go blind is sitting too close to our black and white standard defin...
Reflections on the Growth of 3D Returns After a two month hiatus, Reflections on the Growth of 3D is back, examining the latest adva...
How 'Hugo' Gave One Neuroscientist the Gift of Ste...
Feature Film Critics Who Hate 3D Movies Should Hav...
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redpajama_set_name: RedPajamaCommonCrawl


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Q: CUDA or same something that can be available to intel graphic card? I want to learn GPGPU and CUDA programming. But I know that only Nvidia card support it. My laptop has an Intel HD Graphic Card. So I need to search if it is possible to do GPGPU or something like that with Intel graphic card. Thanks for any information.

A: To develop in CUDA your options are:

*

*Use an NVIDIA GPU - all NVIDIA server, desktop and laptop GPUs support CUDA since around 2006, since your laptop does not have one you could try using one remotely.

*Use PGI CUDA x86, not free but does what you want.

*Use gpuocelot to execute the PTX on the CPU, that's an open-source project in development so YMMV.

A: You cannot do GPGPU on Intel HD Graphics cards today, unless you do shader-based programming (which was common practice in the days before CUDA and OpenCL).
In my experience, the PGI X86 stuff seems to have fallen flat and I'm not aware of anyone using that.  Ocelot is another attempt at the same, but it is very reasearchy and not fully robust at this point.
The only OpenCL compliant devices from Intel are the latest CPUs (Sandy Bridge and Ivy Bridge).
What CPU do you have in your system?

A: CUDA is Nvidia specific as starter. The GPU emulators are always there in CUDA, so you can use them without a graphics card easily, though it will be slow. A faster solution is the
the x86 implementation. Any of these will allow you to learn the basics of CUDA without using the GPU at all.
If you are want to learn GPGPU in general you still have the option to learn OpenCL, which more widely supported, including AMD, Intel, Nvidia etc... E.g. Intel has an OpenCL SDK (the target is the CPU then, but I guess is irrelevant for you).
After learning the basics of either CUDA or OpenCL, the other will be easy to learn. Neither the syntax nor the semantics are the same, but it is easy step forward as the concepts are the same.


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El XLII Campeonato Mundial de Tiro se celebró en Seúl (Corea del Sur) en el año 1978 bajo la organización de la Federación Internacional de Tiro Deportivo (ISSF) y la Federación Surcoreana de Tiro.

Las competiciones se realizaron en el Campo de Tiro Internacional de Taenung de la capital .

Resultados

Masculino

Femenino

Medallero

Enlaces externos
Resultados oficiales en el banco de datos de la ISSF (en inglés)

Campeonatos mundiales de tiro deportivo

redpajama_set_name: RedPajamaWikipedia


The Delta Sky Club ORD food is pretty standard for most Delta Skyclubs � breakfast was oatmeal and grits along with assorted breads / bagels, fruits and yogurt. Around 11 a.m. they switched over to the lunch service which was soup, salad fixings, cheese, hummus, cookies, etc.
26/09/2017�� The Delta Sky Club Tokyo Narita Airport is setup in two identical sections to the right and left of the reception desk. The sections were subdivided into various seating options including tables and chairs, leather chairs as well as computer work stations.


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Lower Power FM Radio Could Offer Immigrant Communities New Way to Communicate
June 17, 2011	/ no comments	/	1808 views
NYC taxi drivers keep in touch using cell phones. (Photo: Colin Milligan/flickr)
In the late 1990s, Pakistani, Indian and other South Asian cab drivers in New York City developed a unique communication system using CB (Citizen's Band) radio to discuss their community's issues in their native tongues.
"I remember there used to be hundreds of drivers on the CB radio and we used to share all kind of information with each other including traffic, weather, customers waiting for the cab, local, international news," recalled Suhail Shabbir, a former driver. "Many times we were tipped of by other drivers that police in certain areas is (sic) stopping and checking the cabs, then we used to change our routes."
In more recent years, conference calls, three-way calling features and unlimited talk plans offered by cell phone companies have filled the communication and information-sharing needs of South Asian cab drivers.
"Most of the drivers are now using cellular phones not only to keep in touch, but to share information, news, views and many other things with each other. The same is the case with other members of our communities," said Shabbir, who no longer drives a cab and now runs his own cell phone business.
Now these communities may be able to move to another means of communication to discuss their issues.
On January 7, 2011 President Obama signed the Local Community Radio Act, which allows for the creation of thousands of new non-commercial stations on U.S. airwaves.
Community radio offers a third model of broadcasting beyond commercial and public service radio. The idea is that community radio stations broadcast content that is popular and relevant to a specific local audience which may be overlooked by commercial or mass-media broadcasters. These non-commercial stations will broadcast local news, independent music, arts and other diverse programming specific to a geographic area or community of interest.
The Federal Communications Commission (FCC) is currently in the process of making rules for Low-Power FM (LPFM) radio stations.
According to the Prometheus Radio Project , a non-profit organization founded by a group of radio activists, "The act's passage is a major victory for community radio, permitting hundreds or thousands of groups to launch LPFM radio stations that will aid their own specific community needs."
"It may take up to a year (the summer of 2012) before the FCC is ready to accept applications," said Brandy Doyle, policy director of the Prometheus Radio Project. "For now, interested groups can start spreading the word, look for local organizations who could run a radio station, and start having conversations about how a radio station might benefit your community."
Carlos Pareja, training and policy director at the People's Production House in New York believes LPFM radio could be a powerful organizing tool for immigrant communities. "The passage of the Community Radio Act creates the potential for immigrants themselves to transform the debate on immigration," he said. "By broadcasting their stories via a powerful and accessible medium like radio, immigrant communities can broaden the discussion around immigration, moving it from one of law enforcement and security to one that includes the many contributions immigrants bring to our society."
Dr. Mujahid Ghazi, managing director of the Asian Broadcasting Network in Chicago agrees. "Radio has always been and still is an effective form of media for immigrant communities like the South Asian community—confronted with language and lack of awareness challenges radio means a lot." Dr. Ghazi who ran "Talk Radio Chicago" for 14 years has recently suspended his radio channel because of a lack of funding.
Some immigrants groups are already using low power radio to serve and connect with their communities. The Coalition of Immokalee Workers runs WCIW to organize Guatemalan farm workers in Immokalee, Florida for fair wages and better working conditions. In Oroville, California the low power station KRBS has a number of programs serving the Hmong community.
"Since the passage of the Local Community Radio Act, we now expect that immigrant communities even in major cities will finally have a chance to apply for stations," said Doyle. "For the first time, groups in cities like Chicago, Seattle, and even New York may have the chance to run their own community radio stations."
But the reach of community radio requires more than airwaves, it also depends on people tuning in. According to Pareja:
"The level of awareness is pretty low in immigrant communities regarding the opportunity for communities to take advantage of this extraordinary communications resource and apply for their own low power FM radio licenses."
He added, "I believe media policy advocates should play a role in this regard."
Janice Wise, an FCC spokesperson, said the agency was taking this into account. "We will do outreach as well as promote the window that will be open to apply for the LPFM radio lisences, on our web pages," she said.
"Immigrant communities need to contact organizations within their communities: faith-based organizations like mosques, churches and others community anchors like employment centers or settlement houses and ask if they're aware of the Community Radio Act," said Mr. Pareja, "Work with them to gauge their capacity to run a radio station or work towards building a neighborhood alliance to take on this grassroots media project."
The ultimate goal is that, "communities will get their own voices in public broadcasting," said Maxie Jackson, president of the National Federation of Community Broadcasters (NFCB), an organization representing 175 stations in the U.S.
"It's a good news for me too, said Dr. Ghazi, "Now I may be able to bring my radio channel, Talk Radio Chicago, back 'On Air' again."
Feet in Two Worlds coverage of media policy is supported by The Media Consortium.
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About Mohsin Zaheer
Mohsin Zaheer is a Pakistani-American journalist and editor based in New York whose work spans two decades. He won the New York Community Media Alliance's Ippies Award in 2009 and has been the beneficiary of numerous Pakistani-American awards. Zaheer joined Daily Khabrain, Lahore (the Urdu-language newspaper with the largest circulation in Pakistan) in 1989 as staff reporter, eventually becoming the Deputy Editor of Reporting. Zaheer moved to the U.S. in 1999 and joined the staff of Sada-e-Pakistan, an Urdu-language weekly, as Editor and set a new trend for Pakistani-American media by reporting on local issues and activities taking place in the U.S. He covered the 9/11 attacks, wide raging issues within the Pakistani-American community in a post 9/11 era, and the relationship between the U.S. and Pakistan. Zaheer also launched the Pakistani American community's first online newspaper in 1996, "The Pakistani Newspaper" (www.pn.com.pk), and continues to contribute news stories and columns to Daily Khabrain, Lahore. Zaheer earned his Master degree in Political Science and History from the University of Punjab in Lahore, Pakistan.
View all posts by Mohsin Zaheer →
De Leon: If E-Verify Becomes Mandatory, It Won't Solve Nation's 'Immigration Problem'
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The Town of Mamaroneck Community Services Office provides information, referral, and assistance to residents seeking affordable housing.
The Housing Choice Voucher Program (also known as "Section 8") is administered by the Town of Mamaroneck PHA. The program is funded by the U.S. Department of Housing and Urban Development (HUD) and provides rental assistance to income‐eligible individuals and families. The Town of Mamaroneck Public Housing Agency (PHA) is authorized by HUD to administer 647 vouchers, however limited funding prevents the PHA from issuing all of the vouchers available.
The Section 8 waiting list is now closed. Only 800 pre-applications have been selected for placement on the waiting list. Results of the lottery are available online now. Your status will only be provided online at www.waitlistcheck.com. Please do not call the Town of Mamaroneck for status information.
If you see that your status is Inactive that means that your pre-application was not selected in the lottery.
If you see that your status is Active, your pre-application was selected in the lottery and has been placed on the waiting list. You may now create an AssistanceCheck account by going to www.assistancecheck.com and using the PIN specified on your application receipt. This will allow you to update information including legal & mailing addresses and family composition online. Any mail sent to you by the Town of Mamaroneck that is returned to us will result in your removal from the waiting list.
Due to limited funding available for housing vouchers, the Town of Mamaroneck cannot give an estimated time frame for when you will be contacted to submit the full application and required documentation.
The Hommocks Park Apartments, located on the corner of the Boston Post Road and Weaver Street is an affordable housing development managed by Gramatan Management. These townhouse-style units each have washer/dryer hook-ups and an individual garage. Additional parking is available on site for tenants and guests. Tenants are responsible for paying all of their utilities. Apartments of varying sizes are available including 1 bedroom, 1 bedroom with loft, 2 bedrooms and 2 bedrooms with loft. Lofts are not permitted to be used as a bedroom. For information on general availability, please call 914-654-1414. The Hommocks Park Apartments complex also has 13 units set aside for Housing Choice Voucher holders, administered by the Town of Mamaroneck PHA.
The Town of Mamaroneck PHA is currently accepting applications ONLINE ONLY for one 1 bedroom unit and one 2 bedroom unit. Grand Street Lofts are located on the corner of Mamaroneck Avenue and Grand Street in Mamaroneck Village.
This waiting list is currently closed.
Please note: There is no rent subsidy associated with these units. Applicants must have sufficient income as described above to be able to afford to pay the rent and the utilities. The rent for a 1 bedroom is $1,706.75; utilities are estimated at $167 per month depending on individual usage. The rent for a 2 bedroom unit is $2,138.25; utilities are estimated at $203 per month depending on individual usage. Tenants must pay all the utilities; all appliances are electric.


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