64 Sentences With "brightnesses" | Random Sentence Generator

Gaia's catalog includes the stars' positions, brightnesses, and colors, plus information about asteroids in our own solar system.

With surface brightnesses up to 250 times fainter than the night sky, these galaxies can be incredibly difficult to detect.

This accounts for the relative brightnesses of both objects, which could not otherwise both be exposed equally in the same shot.

The final Gaia catalog, expected in the early 2020s, will include positions, motions, brightnesses and other parameters of over a billion more stars.

Essentially, HDR TVs are able to display a wider range of brightnesses compared to Standard Dynamic Range (SDR) TVs, going from darker blacks to brighter whites.

You can also change the parameters, shape settings, colors, the brightnesses of the primaries, saturations, and even the parameters according to byte size, ranging from 1-bit upwards.

TESS will measure the brightnesses of nearly 200,000 stars every two minutes, and record an image of the entire swath of sky in the segment every half-hour.

Compared side by side, the old Oasis now looks washed out, with a sickly grey backdrop for the text at lower brightnesses and a corpse-like white at higher ones.

See how Jon (I think) is made up almost entirely of only a handful of different colors (brightnesses of a similar color, really) in with big obvious borders between them?

The researchers said they ruled out cases where the baby was in a deep sleep, but the fetuses could have been lightly sleeping and rousing to different brightnesses of light.

Graphic: Sownak BoseThe researchers developed computer models and simulations to predict how many dwarf galaxies there should be for given brightnesses, according to the paper published today in The Astrophysical Journal.

Some studies have examined the cephalopod's ability to discern objects of different sizes, shapes, colors, brightnesses and textures; and its problem-solving, including the ability to navigate mazes and open jars.

I had become fond of these orange poppiesand their disintegrationforces me to face inevitable endings and renunciationsof all seasons,of all the sunlit fields I ever saw,of all brightnesses, persons, myself.

These devices all have different-sized displays with different max brightnesses, and we want them on as equal a playing field as possible, as the more light the display puts out the faster its battery drains.

Others have adjusted the LED light—which is notoriously shitty in the original, with the bulb shining at a 90 degree angle away from the stuff you actually want illuminated on the face—and added different colors or brightnesses.

Both research teams relied on data from the European Space Agency's Gaia space telescope, which has spent years gathering exceptionally rich biographies of millions of stars—not only their locations and motions, but for many, their brightnesses, temperatures, ages and composition as well.

These included calculations of the surface brightnesses and radii of stars.

Friedrich Wilhelm August Argelander (22 March 1799 – 17 February 1875) was a German astronomer. He is known for his determinations of stellar brightnesses, positions, and distances.

Gilmore has had an important role in the design and scientific strategy of the European Space Agency's Gaia spacecraft that is measuring the positions, motions and brightnesses of millions of stars in the Galaxy.

A model of the SPIRE instrument. Herschel in a clean room ; SPIRE (Spectral and Photometric Imaging Receiver): An imaging camera and low-resolution spectrometer covering 194 to 672 micrometre wavelength. The spectrometer had a resolution between R=40 and R=1000 at a wavelength of 250 micrometres and was able to image point sources with brightnesses around 100 millijanskys (mJy) and extended sources with brightnesses of around 500 mJy. The imaging camera had three bands, centred at 250, 350 and 500 micrometres, each with 139, 88 and 43 pixels respectively.

Desdemona may collide with either Cressida or Juliet within the next 100 million years. The five largest moons of Uranus compared at their proper relative sizes and brightnesses. From left to right (in order of increasing distance from Uranus): Miranda, Ariel, Umbriel, Titania, and Oberon.

For images with a modest range of brightnesses from the darkest to the lightest, eight bits per primary color provides good-quality images, but extreme images require more bits per primary color as well as the advanced display technology. For more information see High Dynamic Range (HDR) imaging.

The Chinese records have some importance to modern science because they allow astronomers to deduce the past orbits and brightnesses of comets. This is important because comet orbits are not always entirely regular. They can be changed by gravitational encounters with the planets. Without ancient records, such past changes would be very difficult to determine.

Calibrator stars close in the sky to the target are favoured (to avoid large differences in the atmospheric paths). If those stars have somewhat different zenith angles (altitudes) then a correction factor as a function of airmass can be derived and applied to the airmass at the target's position. Such calibration obtains the brightnesses as would be observed from above the atmosphere, where apparent magnitude is defined.

At intermediate positions of the second crystal, each ray emerging from the first is doubly refracted by the second, giving four rays in total; and as the crystal is rotated from the initial orientation to the perpendicular one, the brightnesses of the rays vary, giving a smooth transition between the extreme cases in which there are only two final rays.Huygens, 1690, tr. Thompson, pp.92–4.

The brightnesses of the three stars have been measured at visual and infrared wavelengths using adaptive optics. The physical properties implied by their surface brightnesses and colour indices suggests spectral types of A2IV, A4V, and F8V respectively. More precise physical properties for the stars can be calculated using accurate orbital parameters. Both members of the spectroscopic binary Delta Velorum A are slightly evolved stars that are still on the main sequence. Component Aa has 2.5 times the mass of the Sun, 2.6 times the Sun's radius, and is radiating 56 times the luminosity of the Sun at an effective temperature of 9,470. Component Ab is only slightly smaller, with 2.4 times the Sun's mass and radius, with a luminosity of 47 times the Sun and an effective temperature of 9,370 K. Both stars are rotating rapidly and are significantly oblate, with polar radii smaller than their equatorial radii.

The difference between the maximum and minimum brightnesses (the amplitude of the light curve) can be due to the shape of the object, or to bright and dark areas on its surface. For example, an asymmetrical asteroid's light curve generally has more pronounced peaks, while a more spherical object's light curve will be flatter. This allows astronomers to infer information about the shape and spin (but not size) of asteroids.

NGC 5474, an example of a dwarf spiral galaxy A dwarf spiral galaxy is the dwarf version of a spiral galaxy. Dwarf galaxies are characterized as having low luminosities, small diameters (less than 5 kpc), low surface brightnesses, and low hydrogen masses. The galaxies may be considered a subclass of low- surface-brightness galaxies. Dwarf spiral galaxies, particularly the dwarf counterparts of Sa-Sc type spiral galaxies, are quite rare.

During the first half of the 20th century the ROE pursued the new fields of photographic and photoelectric recording of stellar positions, brightnesses and spectra. From the 1950s onwards the ROE has concentrated even more on instrumentation and automation. In 1965 the ROE moved from the responsibility of the Scottish Office into the new Science Research Council (SRC), which in 1981 became the Science and Engineering Research Council (SERC).

32 Comets that actually have a tail can be described as beixing when they are in opposition and the tail is not visible, giving a further clue.Needham, p. 431 Chinese records of comet brightness are superior to Western observations to an even later date. The West did not overtake Chinese astronomers in this respect until the twentieth century, at least in the matter of diligent recording of brightnesses.

Photometric parallax is a means to infer the distances of stars using their colours and apparent brightnesses. It was used by the Sloan Digital Sky Survey to discover the Virgo super star cluster. Assuming that a star is on the main sequence, the star's absolute magnitude can be determined based on its color. Once the absolute and apparent magnitudes are known, the distance to the star can be determined by using the distance modulus.

Dia imaged by the Canada-France-Hawaii Telescope in December 2001. In the second frame Dia is not visible due to Jupiter's glare reducing the relative brightnesses of the stars. Dia was discovered by a team of astronomers from the University of Hawaii led by Scott S. Sheppard in 2000 with an observation arc of 26 days. Initial observations were not followed up, and Dia was not observed for more than a decade after 2000.

Gilmore was educated at St Bede's College, Christchurch and the University of Canterbury, where he was awarded a Bachelor of Science degree in 1973. Gilmore remained at the University of Canterbury as a postgraduate research student. He used the 0.61-metre telescope at Mount John University Observatory to monitor changes in the brightnesses of quasars in the southern hemisphere of the sky. He measured the magnitudes of about 130 quasars from a large number of photographic plates.

Eigenfaces as examples of eigenvectors In image processing, processed images of faces can be seen as vectors whose components are the brightnesses of each pixel. The dimension of this vector space is the number of pixels. The eigenvectors of the covariance matrix associated with a large set of normalized pictures of faces are called eigenfaces; this is an example of principal component analysis. They are very useful for expressing any face image as a linear combination of some of them.

He travelled to Minsk in Eastern Europe in 1914 to observe a total solar eclipse, departing during peacetime but returning after the start of the First World War. His activities at the observatory were disrupted by the war, when he worked temporarily for the Ministry of Munitions, particularly on optics. In 1918 Spencer Jones married Gladys Mary Owers. He resumed his astronomical work after the war, including studying the positions of stars, the rotation of the Earth, and the brightnesses of stars.

He led efforts by the staff to measure the properties of large numbers of stars from photographic plates exposed on the observatory's telescopes. This work included measuring the positions of stars that had been studied years earlier to determine their proper motions (their very small movements across the sky relative to distant stars). The velocities of stars along the line-of-sight were measured from their spectra. The staff members measured brightnesses of 40000 stars from their images on photographs.

She later attributed this lasing to the random scattering of light within the zinc oxide grains. Cao switched her research focus to random lasers, lasers where modes are determined by multiple scattering events. In conventional lasers, high spatial coherence can result in artefacts such as a speckle, which can compromise full-field imaging. Random lasers can achieve similar brightnesses to conventional lasers, but demonstrate low spatial coherence and are much more simple to fabricate: they can even be made using disordered materials.

Kalirai & Richer (2010). Star clusters as laboratories for stellar and dynamical evolution, Philosophical Transactions of the Royal Society A, 368, 1913 Further, the morphology of the cluster stars in a color-magnitude diagram, and that includes the brightnesses of distance indicators such as RR Lyrae variable members, can be influenced by observational biases. One such effect is called blending, and it arises because the cores of globular clusters are so dense that in low-resolution observations multiple (unresolved) stars may appear as a single target.

These charts were computer-plotted by the cartographic company of John Bartholomew and Son Ltd. in Edinburgh, Scotland, taking star positions and brightnesses from the most recent version of the Bright Star Catalogue, the successor to the Harvard Revised Photometry. The total number of stars plotted was over 8800, reaching to magnitude 6.5. The text was extensively rewritten and reorganized under the editorship of the British astronomy writer Ian Ridpath. For the first time in its history, Norton’s Star Atlas contained nothing by Norton himself.

The M81 Group is a galaxy group in the constellations Ursa Major and Camelopardalis that includes the galaxies Messier 81 and Messier 82, as well as several other galaxies with high apparent brightnesses. The approximate center of the group is located at a distance of 3.6 Mpc, making it one of the nearest groups to the Local Group. The group is estimated to have a total mass of (1.03 ± 0.17). The M81 Group, the Local Group, and other nearby groups all lie within the Virgo Supercluster (i.e.

A viewer located in the umbra region cannot directly see any part of the light source. By contrast, the penumbra is illuminated by some parts of the light source, giving it an intermediate level of light intensity. A viewer located in the penumbra region will see the light source, but it is partially blocked by the object casting the shadow. If there is more than one light source, there will be several shadows, with the overlapping parts darker, and various combinations of brightnesses or even colors.

Negative film typically has a gamma less than 1; positive film (slide film, reversal film) typically has a gamma with absolute value greater than 1. Photographic film has a much greater ability to record fine differences in shade than can be reproduced on photographic paper. Similarly, most video screens are not capable of displaying the range of brightnesses (dynamic range) that can be captured by typical electronic cameras. For this reason, considerable artistic effort is invested in choosing the reduced form in which the original image should be presented.

The shapes of variable star light curves give valuable information about the underlying physical processes producing the brightness changes. For eclipsing variables, the shape of the light curve indicates the degree of totality, the relative sizes of the stars, and their relative surface brightnesses. It may also show the eccentricity of the orbit and distortions in the shape of the two stars. For pulsating stars, the amplitude or period of the pulsations can be related to the luminosity of the star, and the light curve shape can be an indicator of the pulsation mode.

Seyfert galaxies are one of the two largest groups of active galaxies, along with quasars. They have quasar-like nuclei (very luminous, distant and bright sources of electromagnetic radiation) with very high surface brightnesses but unlike quasars, their host galaxies are clearly detectable. Seyfert galaxies account for about 10% of all galaxies. Seen in visible light, most Seyfert galaxies look like normal spiral galaxies, but when studied under other wavelengths, the luminosity of their cores is equivalent to the luminosity of whole galaxies the size of the Milky Way.

For the first edition, Norton based his charts on the Uranométrie Générale star catalogue compiled by the Belgian astronomer Jean-Charles Houzeau. Constellation boundaries were represented by dashed lines meandering between the stars, for no official boundaries were then established. For the 5th edition of the Atlas, published in 1933, Norton completely redrew the charts, despite now suffering from severely impaired vision in his left eye due to a blood clot behind the retina. This time he used the Harvard Revised Photometry catalogue for the positions and brightnesses of the stars.

He has made a long study of visual inhibition, the process whereby a neuron firing in response to one group of retinal cells can inhibit the firing of another neuron; this allows perception of relative contrast. In 1961, Barlow wrote a seminal article where he asked what the computational aims of the visual system are. He concluded that one of the main aims of visual processing is the reduction of redundancy. While the brightnesses of neighbouring points in images are usually very similar, the retina reduces this redundancy.

In a widely admired paper published in 1948,Wallach, H. (1948) Brightness constancy and the nature of achromatic colors. Journal of Experimental Psychology, 38, 310–324. Wallach explored the stimulus conditions for the perception of neutral colors – that is, colors that vary in lightness but have no hue, thus ranging from white to gray to black. Wallach projected round patches of light (“disks”) of various brightnesses on a white screen in a dark room and found that, when presented alone, the disks always appeared to be luminous – i.e.

A comparison between a typical normalized M cone's spectral sensitivity and the CIE 1931 luminosity function for a standard observer in photopic vision. When judging the relative luminance (brightness) of different colors in well-lit situations, humans tend to perceive light within the green parts of the spectrum as brighter than red or blue light of equal power. The luminosity function that describes the perceived brightnesses of different wavelengths is thus roughly analogous to the spectral sensitivity of M cones. The CIE model capitalizes on this fact by setting Y as luminance.

In astronomy, color–color diagrams are a means of comparing the apparent magnitudes of stars at different wavelengths. Astronomers typically observe at narrow bands around certain wavelengths, and objects observed will have different brightnesses in each band. The difference in brightness between two bands is referred to as color. On color–color diagrams, the color defined by two wavelength bands is plotted on the horizontal axis, and then the color defined by another brightness difference (though usually there is one band involved in determining both colors) will be plotted on the vertical axis.

Hipparcos was a scientific satellite of the European Space Agency (ESA), launched in 1989 and operated until 1993. It was the first space experiment devoted to precision astrometry, the accurate measurement of the positions of celestial objects on the sky. This permitted the first high-precision measurements of the intrinsic brightnesses (compared to the less precise apparent brightness), proper motions and parallaxes of stars, enabling better calculations of their distance and tangential velocity. When combined with radial velocity measurements from spectroscopy, astrophysicists were able to finally measure all six quantities needed to determine the motion of stars.

Its blue color points to a particle radius near 10 nm, but the ratio of brightnesses at different phase angles indicates a radius exceeding 100 nm. This can be explained by aggregation of small (tens of nm) particles into larger (hundreds of nm) clusters. The haze probably consists of particles of non-volatile compounds, which are synthesized from atmospheric gases under influence of cosmic high-energy radiation. The layers show the presence of atmospheric waves (presence of which is also suggested by observations of occultations), and such waves can be created by wind blowing over Pluto's rough surface.

In the early 2000s, infrared images in the J, H, and Ks bands have suggested at least 350 cluster members. Observations by NASA's Spitzer Space Telescope and Chandra X-ray Observatory were used to identify cluster members as part of the MYStIX survey of nearby star-forming regions. In the MYStIX catalog of 384 probable young stellar members of RCW 36, more than 300 of the stars are detected by X-ray sources. Modeling of the brightnesses of stars at various infrared wavelengths has shown 132 young stellar objects to have infrared excess consistent with circumstellar disks or envelopes.

Despite the radii of dSphs being much larger than those of globular clusters, they are much more difficult to find due to their low luminosities and surface brightnesses. Dwarf spheroidal galaxies have a large range of luminosities, and known dwarf spheroidal galaxies span several orders of magnitude of luminosity. Their luminosities are so low that Ursa Minor, Carina, and Draco, the known dwarf spheroidal galaxies with the lowest luminosities, have mass-to-light ratios (M/L) greater than that of the Milky Way. Dwarf spheroidals also have little to no gas with no obvious signs of recent star formation.

Gerry Gilmore worked as a research fellow at the Royal Observatory, Edinburgh, Scotland, between 1979 and 1984. He used the expertise gained during his PhD to measure brightnesses and numbers of stars from photographic sky surveys. Working with Neil Reid with data from the United Kingdom Schmidt Telescope, he found an excess of faint stars compared to standard models of the Galaxy that represented the distribution of stars as two simple components. Gilmore and Reid argued the observed numbers of stars implied the existence of an additional component they called the thick disc that exists alongside the main Galactic disc and the stellar halo.

Mesh merging is more precise and is the final step in visualizing the unwrapped scroll. This type of merging recombines each point on the surface of each segment with the corresponding point on its neighbor segment to remove the distortions due to individual flattening. This step also re-flattens and re- textures the image to create the final visualization of the unwrapped scroll, and is computationally expensive compared to the texture merging process detailed above. Using each of these steps, the computer is able to transform the voxels from the 3D volumetric scan and their corresponding density brightnesses to a 2D virtually unwrapped image of the text inside.

Brightness, as it is most often used in marketing literature, refers to the emitted luminous intensity on screen, measured in candela per square metre (cd/m2). The higher the number, the brighter the screen. It is also common to market only the dynamic contrast ratio capability of a display (when it is better than its static contrast ratio only on paper), which should not be directly compared to the static contrast ratio. A plasma display with a 4,000,000:1 static contrast ratio will show superior contrast to an LCD (with LED or CCFL backlight) with 30,000,000:1 dynamic and 20,000:1 static contrast ratio when the input signal contains a full range of brightnesses from 0 to 100% simultaneously.

In addition to the 1986U2R/ζ and λ rings, there are other extremely faint dust bands in the Uranian ring system. They are invisible during occultations because they have negligible optical depth, though they are bright in forward-scattered light. Voyager 2's images of forward-scattered light revealed the existence of bright dust bands between the λ and δ rings, between the η and β rings, and between the α ring and ring 4. Many of these bands were detected again in 2003–2004 by the Keck Telescope and during the 2007 ring-plane crossing event in backscattered light, but their precise locations and relative brightnesses were different from during the Voyager observations.

The Circinus Galaxy, a Type II Seyfert galaxy Seyfert galaxies are one of the two largest groups of active galaxies, along with quasars. They have quasar- like nuclei (very luminous, distant and bright sources of electromagnetic radiation) with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, their host galaxies are clearly detectable. Seyfert galaxies account for about 10% of all galaxies and are some of the most intensely studied objects in astronomy, as they are thought to be powered by the same phenomena that occur in quasars, although they are closer and less luminous than quasars. These galaxies have supermassive black holes at their centers which are surrounded by accretion discs of in-falling material.

The primary star is also unusual in that it does not exhibit internal seismic oscillations as have been detected in other red giants, although tidal forces from the closer pair may possibly be causing other variability in the light curve of the system. HD 181068 Ba and Bb have spectral types of G8V and K1V respectively, indicating their location on the main sequence, slightly later than the Sun. They are in a close orbit and complete an orbit once every 0.906 days (about 21.7 hours), while they orbit HD 181068 A every 45.5 days. All three stars have similar surface brightnesses and colors, so when the two companions eclipse the red giant, the change in brightness is very slight and hard to detect.

JPL News reported that Oumuamua "is up to one-quarter mile, , long and highly-elongated-perhaps 10 times as long as it is wide". A 2019 paper finds the best models as either a cigar-shape, 1:8 aspect ratio, or disc-shape, 1:6 aspect ratio, with the disc more likely since its rotation doesn't require a specific orientation to see the range of brightnesses observed. Monte Carlo simulations based on the available orbit determination suggest that the equatorial obliquity of Oumuamua could be about 93 degrees, if it has a very prolate or cigar-like shape, or close to 16 degrees, if it is very oblate or disk-like. Light curve observations suggest the object may be composed of dense metal-rich rock that has been reddened by millions of years of exposure to cosmic rays.

Gersonides is the only astronomer before modern times to have estimated correctly stellar distances. Whereas all other astronomers put the stars on a rotating sphere just beyond the outer planets, Gersonides estimated the distance to the stars to be ten billion times greater, of the order of 100 light-years (in modern units). Using data he collected from his own observations, Gersonides refuted Ptolemy's model in what the notable physicist Yuval Ne'eman has considered as "one of the most important insights in the history of science, generally missed in telling the story of the transition from epicyclic corrections to the geocentric model to Copernicus' heliocentric model". Ne'eman argued that after Gersonides reviewed Ptolemy's model with its epicycles he realized that it could be checked, by measuring the changes in the apparent brightnesses of Mars and looking for cyclical changes along the conjectured epicycles.

After a music interlude, and accompanied by her entourage, 8 musicians and 10 dancers, the show continues with "Boomerang" and "Tu Revolución" and leaves the stage. Espósito comes back to the stage to perform a medley of ballads from her previous record A Bailar which includes "Del Otro Lado", "Cielo Salvador" and "Desamor". The ballad act continues as the singer performs "Cree en Mí", creating an intimate atmosphere dominated by red and yellow lights, in which Espósito deploys all her glamor wearing a long dress, with transparencies and brightnesses. The next songs to be performed are "Bomba", in which twerking predominates as dance style, and "Mi Religión", while Espósito descends from the ceiling by commanding a DJ console surrounded by lights, smoke and special effects, which is described as "a 100% energetic moment that brings everyone to their feet for a party-like atmosphere".

Their angular radii have been directly measured; in combination with the very accurate distance, this gives and for Aa and Ab respectively. Their surface temperatures can be calculated by comparison of observed and synthetic spectra, direct measurement of their angular diameters and brightnesses, calibration against their observed colour indices, and disentangling of high resolution spectra. Weighted averages of these four methods give 4,970 ± 50 K for Aa and 5,730 ± 60 for Ab. Their bolometric luminosities are most accurately derived from their apparent magnitudes and bolometric corrections, but are confirmed by calculation from the temperatures and radii of the stars. Aa is 78.7 ± 4.2 times as luminous as the Sun and Ab 72.7 ± 3.6 times as luminous, so the star defined as the primary component is the more luminous when all wavelengths are considered but very slightly less bright at visual wavelengths. Estimated to be 590 to 650 million years old, the stars were probably at the hot end of spectral class A during their main sequence lifetime, similar to Vega.