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Shibori kimono.  Taisho period (1912-1926), Japan.  The Kimono Gallery. A silk shibori kimono featuring large ‘yabane’ (arrow-feather) motifs of shibori with silk and metallic thread embroidery highlights. This kimono is patterned entirely in fine shibori (tie-die). The arrow feather (yabane) motif first became fashionable in Japan as early as the Heian era – initially with martial connotations – and during the Edo era it was often used on kimono for ladies in waiting. The motif was very popular on schoolgirl and teacher kasuri (ikat) kimonos of the mid to late Meiji period. During the Taisho and early Showa periods the yabane was a popular woman’s kimono motif, created via shibori, stenciling, or yuzen-dyeing. The arrow-feather motifs were most often vertical, but sometimes created at an angle, as in this example. The Yabane pattern, like most geometric motifs, is all-season, however, it has an auspicious association with weddings – like an arrow shot from a bow a bride does not return to her parents’ house. This kimono would have been very expensive to create - the shibori work itself would have taken a few months to complete. The white silk embroidery on the two arrow-feather motifs situated on lower left of the kimono is very visible from a distance, and provides a tasteful change from the other plainer motifs. The motifs are randomly scattered throughout the kimono 'canvas’, resulting in a casual relaxed atmosphere. The “speckled” appearance of the yellow background color is an accomplished effect: many thousands of tie-dye knots were once placed here to be able to achieve the slightly puckered yellow dots on black background speckled look.

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Fire beneath the Stars. Volcano, HI.

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Caminhos.

Kimono. Taisho to early Showa period (1912-1939), Japan. A fine rinzu (damask) silk kimono featuring carp created with metallic thread weaving. Silk lining. This kimono reflects the experimentation with tradition during the Taisho period and early Showa period; the artist in this example has taken the traditional auspicious carp motif, placing them under bold lavender color bands running in parallel angles, to produce a ‘modern’ graphic result.  The Kimono Gallery

Kiyoshi Saitō  斎藤 清 (1907 - 1997) Child in Aizu, c.1947

A Lua Entre as nuvens De uma noite Suave Brisa Cheirosa

Lentes gravitacionais.

What is Gravitational Lensing?

A gravitational lens is a distribution of matter (such as a cluster of galaxies) between a distant light source and an observer, that is capable of bending the light from the source as the light travels towards the observer. This effect is known as gravitational lensing, and the amount of bending is one of the predictions of Albert Einstein’s general theory of relativity.

This illustration shows how gravitational lensing works. The gravity of a large galaxy cluster is so strong, it bends, brightens and distorts the light of distant galaxies behind it. The scale has been greatly exaggerated; in reality, the distant galaxy is much further away and much smaller. Credit: NASA, ESA, L. Calcada

There are three classes of gravitational lensing:

1° Strong lensing: where there are easily visible distortions such as the formation of Einstein rings, arcs, and multiple images.

Einstein ring. credit: NASA/ESA&Hubble

2° Weak lensing: where the distortions of background sources are much smaller and can only be detected by analyzing large numbers of sources in a statistical way to find coherent distortions of only a few percent. The lensing shows up statistically as a preferred stretching of the background objects perpendicular to the direction to the centre of the lens. By measuring the shapes and orientations of large numbers of distant galaxies, their orientations can be averaged to measure the shear of the lensing field in any region. This, in turn, can be used to reconstruct the mass distribution in the area: in particular, the background distribution of dark matter can be reconstructed. Since galaxies are intrinsically elliptical and the weak gravitational lensing signal is small, a very large number of galaxies must be used in these surveys.

The effects of foreground galaxy cluster mass on background galaxy shapes. The upper left panel shows (projected onto the plane of the sky) the shapes of cluster members (in yellow) and background galaxies (in white), ignoring the effects of weak lensing. The lower right panel shows this same scenario, but includes the effects of lensing. The middle panel shows a 3-d representation of the positions of cluster and source galaxies, relative to the observer. Note that the background galaxies appear stretched tangentially around the cluster.

3° Microlensing: where no distortion in shape can be seen but the amount of light received from a background object changes in time. The lensing object may be stars in the Milky Way in one typical case, with the background source being stars in a remote galaxy, or, in another case, an even more distant quasar. The effect is small, such that (in the case of strong lensing) even a galaxy with a mass more than 100 billion times that of the Sun will produce multiple images separated by only a few arcseconds. Galaxy clusters can produce separations of several arcminutes. In both cases the galaxies and sources are quite distant, many hundreds of megaparsecs away from our Galaxy.

Gravitational lenses act equally on all kinds of electromagnetic radiation, not just visible light. Weak lensing effects are being studied for the cosmic microwave background as well as galaxy surveys. Strong lenses have been observed in radio and x-ray regimes as well. If a strong lens produces multiple images, there will be a relative time delay between two paths: that is, in one image the lensed object will be observed before the other image.

As an exoplanet passes in front of a more distant star, its gravity causes the trajectory of the starlight to bend, and in some cases results in a brief brightening of the background star as seen by a telescope. The artistic concept illustrates this effect. This phenomenon of gravitational microlensing enables scientists to search for exoplanets that are too distant and dark to detect any other way.Credits: NASA Ames/JPL-Caltech/T. Pyle

Explanation in terms of space–time curvature

Simulated gravitational lensing by black hole by: Earther

In general relativity, light follows the curvature of spacetime, hence when light passes around a massive object, it is bent. This means that the light from an object on the other side will be bent towards an observer’s eye, just like an ordinary lens. In General Relativity the speed of light depends on the gravitational potential (aka the metric) and this bending can be viewed as a consequence of the light traveling along a gradient in light speed. Light rays are the boundary between the future, the spacelike, and the past regions. The gravitational attraction can be viewed as the motion of undisturbed objects in a background curved geometry or alternatively as the response of objects to a force in a flat geometry.

A galaxy perfectly aligned with a supernova (supernova PS1-10afx) acts as a cosmic magnifying glass, making it appear 100 billion times more dazzling than our Sun. Image credit: Anupreeta More/Kavli IPMU.

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