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Tracklist: 1. 67000 MPH 2. Ok Chorale 3. Stillness 4. Kite For Seamus 5. Just 4 Now 6. Ayu 7. A Silver Moon 8. Manioc Maniac 9. Rabat

This article is from Scientific Reports , volume 4 . Abstract In electronic holography, various methods have been considered for using multiple spatial light modulators (SLM) to increase the image size. In a previous work, we used a monochrome light source for a method that located an optical system containing lens arrays and other components in front of multiple SLMs. This paper proposes a colourization technique for that system based on time division multiplexing using laser light sources of three colours (red, green, and blue). The experimental device we constructed was able to perform video playback (20 fps) in colour of full parallax holographic three-dimensional (3D) images with an image size of 63 mm and a viewing-zone angle of 5.6 degrees without losing any part of the 3D image.

(REMIX )  Parallax by Hazel C64 Music remake 

On the Parallax of a Lyrae. Pond, J Abstracts of the Papers Printed in the Philosophical Transactions of the Royal Society of London (1800-1843). 1815-01-01. 2:184–185

Concise Rules for Computing the Effects of Refraction and Parallax in Varying the Apparent Distance of the Moon from the Sun or a Star; Also an Easy Rule of Approximation for Computing the Distance of the Moon from a Star, the Longitudes and Latitudes of Both Being Given, with Demonstrations of the Same: By the Rev. Nevil Maskelyne, A. M. Fellow of Trinity College, in the University of Cambridge, and F. R. S Maskelyne, N Philosophical Transactions (1683-1775). 1764-01-01. 54:263–276

Remarks on the Parallax of $\alpha $ Lyrae. Brinkley, J Philosophical Transactions of the Royal Society of London (1776-1886). 1824-01-01. 114:471–498

On the Results of Periodical Observations of the Positions and Distances of Nineteen of the Stars in Sir John Herschel's Lists of Stars, Favourably Situated for the Investigation of Parallax, Contained in Part III. Of the Philosophical Transactions for 1826, and Part I. 1827. Wrottesley, L Philosophical Transactions of the Royal Society of London (1776-1886). 1851-01-01. 141:333–356

A Discourse on the Parallax of the Sun. By the Rev. Thomas Hornsby, M. A. Savilian Professor of Astronomy in the University of Oxford, and F. R. S Hornsby, T Philosophical Transactions (1683-1775). 1763-01-01. 53:467–495

Weisberg, an Office of Strategic Services officer during World War II, U.S. Senate staff member and investigative reporter, devoted 40 years of his life to researching and writing about the Kennedy and King assassinations. His first book, Whitewash: The Report on the Warren Report (1965), was the first critical study of the government's official version of what happened in Dallas on Nov. 22, 1963. Seven of the eight books Weisberg published after Whitewash were about the Kennedy assassination. Over time, Weisberg became recognized, both nationally and internationally, as the dean of writers critical of the official version of the JFK assassination known as the Warren Commission Report. Harold Weisberg donated the world's largest accessible private collection of government documents and public records relating to the assassination of President John F. Kennedy to Hood College and the Beneficial-Hodson Library at Hood College, which donated a copy to the National Security Internet Archive.

An ambitious reporter investigates a series of political assassinations. Warren Beatty Hume Cronyn William Daniels Paula Prentiss

https://www.youtube.com/@PoxPopuli

https://www.youtube.com/@PoxPopuli

Just a fun low-key project Source: https://soundcloud.com/stereo-prism/parallax-theory Uploader: STEREOPRISM

An Inquiry into the Probable Parallax, and Magnitude of the Fixed Stars, from the Quantity of Light Which They Afford us, and the Particular Circumstances of Their Situation, by the Rev. John Michell, B. D. F. R. S Michell, J Philosophical Transactions (1683-1775). 1767-01-01. 57:234–264

A near real-time, full parallax holographic display system was developed that has the potential to provide a 3-D display for remote handling operations in hazardous environments. The major components of the system consist of a stack of three spatial light modulators which serves as the object source of the hologram; a near real-time holographic recording material (such as thermoplastic and photopolymer); and an optical system for relaying SLM images to the holographic recording material and to the observer for viewing.

Tom Paynter CCP concert May 19, 1995 Parallax Discontinuance John Hungerford-Shirley: Quintet for strings and computer Tim Edwards: Portrait of a Moment Larry Schenker: Shuffle Ricardo Lorenz: Zamnro tumbo Mirage (gets cut off) (Maybe dupe with TP_037) Shirley Blankenship violin excursions on Guido tunes

We present new statistical parallax solutions for the absolute magnitude and kinematics of RR Lyrae stars. New proper motion, radial velocity, and abundance data are used; the new data set is 50% larger, and of higher quality, than previously available data sets. Based on an a priori kinematic study, we separate the stars into halo and thick disk sub-populations. Statistical parallax solutions on these sub-samples yield M_V(RR) = +0.71 +/- 0.12 at = -1.61 for the halo (162 stars), and M_V(RR) = +0.79 +/- 0.30 at = -0.76 for the thick disk (51 stars). The solutions yield kinematic parameters (solar motion and velocity ellipsoid) in good agreement with estimates of the halo and thick disk kinematics derived from both RR Lyrae stars and other stellar tracers. Monte Carlo simulations indicate that the solutions are accurate, and that the errors may be smaller than the estimates above. The simulations reveal a small bias in the disk solutions, and appropriate corrections are derived. The large uncertainty in the disk M_V(RR) prevents ascertaining the slope of the M_V(RR)-[Fe/H] relation. We find that (1) the distance to the Galactic Center is 7.6 +/- 0.4 kpc; (2) the mean age of the 17 oldest Galactic globular clusters is 16.5 _{-1.9}^{+2.1} Gyr; and (3) the distance modulus of the LMC is 18.28 +/- 0.13 mag. Estimates of H_0 which are based on an LMC distance modulus of 18.50 (e.g., Cepheid studies) increase by 10% if they are recalibrated to match our LMC distance modulus.

We use a Bayesian approach to derive the distance probability distribution for one object from its parallax with measurement uncertainty for two spatial distribution priors, viz. a homogeneous spherical distribution and a galactocentric distribution - applicable for radio pulsars - observed from Earth. We investigate the dependence on measurement uncertainty, and show that a parallax measurement can underestimate or overestimate the actual distance, depending on the spatial distribution prior. We derive the probability distributions for distance and luminosity combined, and for each separately, when a flux with measurement error for the object is also available, and demonstrate the necessity of and dependence on the luminosity function prior. We apply this to estimate the distance and the radio and gamma-ray luminosities of PSR J0218+4232. The use of realistic priors improves the quality of the estimates for distance and luminosity, compared to those based on measurement only. Use of a wrong prior, for example a homogeneous spatial distribution without upper bound, may lead to very wrong results.

We report the discovery of a microlensing planet OGLE-2012-BLG-0950Lb with the planet/host mass ratio of $q \sim 2 \times 10^{-4}$. A long term distortion detected in both MOA and OGLE light curve can be explained by the microlens parallax due to the Earth's orbital motion around the Sun. Although the finite source effect is not detected, we obtain the lens flux by the high resolution Keck AO observation. Combining the microlens parallax and the lens flux reveal the nature of the lens: a planet with mass of $M_{\rm p} = 35^{+17}_{-9} M_{\oplus}$ is orbiting around a M-dwarf with mass of $M_{\rm host} = 0.56^{+0.12}_{-0.16} M_{\odot}$ with a planet-host projected separation of $r_{\perp} =2.7^{+0.6}_{-0.7}$ AU located at $D_{\rm L} = 3.0^{+0.8}_{-1.1}$ kpc from us. This is the first mass measurement from only microlens parallax and the lens flux without the finite source effect. In the coming space observation-era with $Spitzer$, $K2$, $Euclid$, and $WFIRST$, we expect many such events for which we will not be able to measure any finite source effect. This work demonstrates an ability of mass measurements in such events.

We report measurement of trigonometric parallax of IRAS 05168+3634 with VERA. The parallax is 0.532 +/- 0.053 mas, corresponding to a distance of 1.88+0.21/-0.17 kpc. This result is significantly smaller than the previous distance estimate of 6 kpc based on kinematic distance. This drastic change in the source distance revises not only physical parameters of IRAS 05168+3634, but also its location of the source, placing it in the Perseus arm rather than the Outer arm. We also measure proper motions of the source. A combination of the distance and the proper motions with systemic velocity yields rotation velocity ({\Theta}) of 227+9/-11 km s-1 at the source, assuming {\Theta}0 = 240 km s-1. Our result combined with previous VLBI results for six sources in the Perseus arm indicates that the sources rotate systematically slower than the Galactic rotation velocity at the LSR. In fact, we show observed disk peculiar motions averaged over the seven sources in the Perseus arm as (Umean, Vmean) = (11 +/- 3, -17 +/- 3) km s-1, indicating that these seven sources are systematically moving toward the Galactic center, and lag behind the Galactic rotation.

We report on 12 years of observations of PSR J1713+0747, a pulsar in a 68-day orbit with a white dwarf. Pulse times of arrival were measured with uncertainties as small as 200 ns. The timing data yielded measurements of the relativistic Shapiro delay, perturbations of pulsar orbital elements due to secular and annual motion of the Earth, and the pulsar's parallax, as well as pulse spin-down, astrometric, and Keplerian measurements. The observations constrain the masses of the pulsar and secondary star to be m1=1.3+-0.2 solar masses and m2=0.28+-0.03 solar masses, respectively (68% confidence). Combining the theoretical orbital period-core mass relation with the observational constraints yields a somewhat higher pulsar mass, m1=1.53-0.06+0.08 solar masses. The parallax is 0.89+-0.08 mas, corresponding to a distance of 1.1+-0.1 kpc; the precision of the parallax measurement is limited by uncertainties in the electron content of the solar wind. The transverse velocity is unusually small, 33+-3 km/s. We find significant timing noise on time scales of several years, but no more than expected by extrapolating timing noise statistics from the slow pulsar population. With the orientation of the binary orbit fully measured, we are able to improve on previous tests of equivalence principle violations.

I'm a huge fan of the Parallax Propeller microcontroller, so while I was using the logo in another project, I thought "hey, why not print a 3D beanie emblem and stick it on my office door?" So, that's what I did, and here it is. The picture shown was printed at 75% scale and 0.3mm layers (IIRC). The raw logo is also included, in case you'd like to use it in another project.

I'm a huge fan of the Parallax Propeller microcontroller, so while I was using the logo in another project, I thought "hey, why not print a 3D beanie emblem and stick it on my office door?" So, that's what I did, and here it is. The picture shown was printed at 75% scale and 0.3mm layers (IIRC). The raw logo is also included, in case you'd like to use it in another project.

This paper is in the public domain in USA. Metadata comes from the CrossRef API, see full record in the source URL below.

This paper is in the public domain in USA. Metadata comes from the CrossRef API, see full record in the source URL below.

This paper is in the public domain in USA. Metadata comes from the CrossRef API, see full record in the source URL below.

Music from Parallax (19xx)(Seven Up Crew)

The second episode of Parallax View, the weekly podcast of Parallaxi Magazine

Parallax (1986)(Ocean)[cr Sharks][Docs]

Atlas Sound

Name: Parallax Bars Released by: Starr Type: C64 One-File Demo Release Date: 1987 Credits: Code  ....  Starr Music  ....  Rob Hubbard Info from CSDB. Original Entry

Parallax Plus (1987)(Huddy)

A PBR tessellation shader for planetary textures Homepage: https://forum.kerbalspaceprogram.com/index.php?/topic/197024-* Repository: https://github.com/Gameslinx/Tessellation License(s): CC-BY-NC-ND-4.0

Parallax textures for the stock planets Homepage: https://forum.kerbalspaceprogram.com/index.php?/topic/197024-* Repository: https://github.com/Gameslinx/Tessellation License(s): CC-BY-NC-ND-4.0

Parallax_v0.0.4

This paper is in the public domain in USA. Metadata comes from the CrossRef API, see full record in the source URL below.

This paper is in the public domain in USA. Metadata comes from the CrossRef API, see full record in the source URL below.

This paper is in the public domain in USA. Metadata comes from the CrossRef API, see full record in the source URL below.

This paper is in the public domain in USA. Metadata comes from the CrossRef API, see full record in the source URL below.

On the Parallax of the Fixed Stars. Pond, J Abstracts of the Papers Printed in the Philosophical Transactions of the Royal Society of London (1800-1843). 1815-01-01. 2:79–79

Vinyl Rip of the  Progrssive Metal Magnum Opus triple album separated arbitrarily into two parts, unified. 

This paper is in the public domain in USA. Metadata comes from the CrossRef API, see full record in the source URL below.

This paper is in the public domain in USA. Metadata comes from the CrossRef API, see full record in the source URL below.

We have used the Japanese VLBI array VERA to perform high-precision astrometry of an H2O maser source in the Galactic star-forming region NGC 281 West, which has been considered to be part of a 300-pc superbubble. We successfully detected a trigonometric parallax of 0.355+/-0.030 mas, corresponding to a source distance of 2.82+/-0.24 kpc. Our direct distance determination of NGC 281 has resolved the large distance discrepancy between previous photometric and kinematic studies; likely NGC 281 is in the far side of the Perseus spiral arm. The source distance as well as the absolute proper motions were used to demonstrate the 3D structure and expansion of the NGC 281 superbubble, ~650 pc in size parallel to the Galactic disk and with a shape slightly elongated along the disk or spherical, but not vertically elongated, indicating the superbubble expansion may be confined to the disk. We estimate the expansion velocity of the superbubble as ~20 km/s both perpendicular to and parallel to the Galactic disk with a consistent timescale of ~20 Myr.

RXJ1856 and RXJ0720 are the only young isolated radio-quiet neutron stars (NSs) for which trigonometric parallaxes were measured. Due to detection of their thermal emission in X-rays they are important to study NS cooling and to probe theoretical cooling models. Hence, a precise determination of their age is essential. Recently, new parallax measurements of RXJ1856 and RXJ0720 were obtained. Considering that NSs may originate from binary systems that got disrupted due to an asymmetric supernova, we attempt to identify runaway stars which may have been former companions to the NS progenitors. Such an identification would strongly support a particular birth scenario with time and place. We trace back each NS, runaway star and the centres of possible birth associations to find close encounters. The kinematic age is then given by the time since the encounter. We use Monte Carlo simulations to account for observational uncertainties. Using the most recent parallax measurement of 8.16+/-0.80 mas for RXJ1856, we find that it originated in the U Sco association 0.46+/-0.05 Myr ago. This is slightly larger than the value we reported earlier (0.3 Myr). Our result is strongly supported by its current radial velocity that we predict to be 6+19-20 km/s. This implies an inclination angle of 88+/-6 deg consistent with the bow shock. No suitable runaway star was found to be a potential former companion of RXJ1856. Making use of a recent parallax measurement for RXJ0720 of 3.6+/-1.6 mas, we find that this NS was possibly born in Tr 10 0.85+/-0.15 Myr ago. This is somewhat larger than the one obtained using the old parallax value (0.5 Myr). We suggest the B0 runaway supergiant HIP 43158 as a candidate for a former companion. Then, the current distance of RXJ0720 to the Sun should be 286+27-23 pc, in agreement with recent measurements. We then expect the radial velocity of RXJ0720 to be -76+34-17 km/s.

"Note on the Use of the Geometrical Mean Parallax" is an article from Publications of the Astronomical Society of the Pacific, Volume 32 . View more articles from Publications of the Astronomical Society of the Pacific . View this article on JSTOR . View this article's JSTOR metadata . You may also retrieve all of this items metadata in JSON at the following URL: https://archive.org/metadata/jstor-40692200

"The Parallax of B. D. + 36° 3956" is an article from Publications of the Astronomical Society of the Pacific, Volume 30 . View more articles from Publications of the Astronomical Society of the Pacific . View this article on JSTOR . View this article's JSTOR metadata . You may also retrieve all of this items metadata in JSON at the following URL: https://archive.org/metadata/jstor-40710142

"The Parallax of N. G. C. 226" is an article from Publications of the Astronomical Society of the Pacific, Volume 33 . View more articles from Publications of the Astronomical Society of the Pacific . View this article on JSTOR . View this article's JSTOR metadata . You may also retrieve all of this items metadata in JSON at the following URL: https://archive.org/metadata/jstor-40710646

After Effect

Desmistificando Markovian Parallax Denigrate