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Kepler space telescope

The Kepler space telescope is a defunct space telescope launched by NASA in 2009 to discover Earth-sized planets orbiting other stars. Named after astronomer Johannes Kepler, the spacecraft was launched into an Earth-trailing heliocentric orbit. The principal investigator was William J. Borucki. After nine and a half years of operation, the telescope's reaction control system fuel was depleted, and NASA announced its retirement on October 30, 2018.

Designed to survey a portion of Earth's region of the Milky Way to discover Earth-size exoplanets in or near habitable zones and estimate how many of the billions of stars in the Milky Way have such planets, Kepler's sole scientific instrument is a photometer that continually monitored the brightness of approximately 150,000 main sequence stars in a fixed field of view. These data were transmitted to Earth, then analyzed to detect periodic dimming caused by exoplanets that cross in front of their host star. Only planets whose orbits are seen edge-on from Earth could be detected. Kepler observed 530,506 stars and detected 2,778 confirmed planets as of June 16, 2023.

Pre-launch development
The Kepler space telescope was part of NASA's Discovery Program of relatively low-cost science missions. The telescope's construction and initial operation were managed by NASA's Jet Propulsion Laboratory, with Ball Aerospace responsible for developing the Kepler flight system.

In January 2006, the project's launch was delayed eight months because of budget cuts and consolidation at NASA. It was delayed again by four months in March 2006 due to fiscal problems. At this time, the high-gain antenna was changed from a design using a gimbal to one fixed to the frame of the spacecraft to reduce cost and complexity, at the cost of one observation day per month.

Post launch
The Ames Research Center was responsible for the ground system development, mission operations since December 2009, and scientific data analysis. The initial planned lifetime was three and a half years, but greater-than-expected noise in the data, from both the stars and the spacecraft, meant additional time was needed to fulfill all mission goals. Initially, in 2012, the mission was expected to be extended until 2016, but on July 14, 2012, one of the four reaction wheels used for pointing the spacecraft stopped turning, and completing the mission would only be possible if the other three all remained reliable. Then, on May 11, 2013, a second one failed, disabling the collection of science data and threatening the continuation of the mission.

On August 15, 2013, NASA announced that they had given up trying to fix the two failed reaction wheels. This meant the current mission needed to be modified, but it did not necessarily mean the end of planet hunting. NASA had asked the space science community to propose alternative mission plans "potentially including an exoplanet search, using the remaining two good reaction wheels and thrusters". On November 18, 2013, the K2 "Second Light" proposal was reported. This would include utilizing the disabled Kepler in a way that could detect habitable planets around smaller, dimmer red dwarfs. On May 16, 2014, NASA announced the approval of the K2 extension.

By January 2015, Kepler and its follow-up observations had found 1,013 confirmed exoplanets in about 440 star systems, along with a further 3,199 unconfirmed planet candidates. Four planets have been confirmed through Kepler's K2 mission. In November 2013, astronomers estimated, based on Kepler space mission data, that there could be as many as 40 billion rocky Earth-size exoplanets orbiting in the habitable zones of Sun-like stars and red dwarfs within the Milky Way. It is estimated that 11 billion of these planets may be orbiting Sun-like stars. The nearest such planet may be 12 ly away, according to the scientists.

On January 6, 2015, NASA announced the 1,000th confirmed exoplanet discovered by the Kepler space telescope. Four of the newly confirmed exoplanets were found to orbit within habitable zones of their related stars: three of the four, Kepler-438b, Kepler-442b and Kepler-452b, are almost Earth-size and likely rocky; the fourth, Kepler-440b, is a super-Earth. On May 10, 2016, NASA verified 1,284 new exoplanets found by Kepler, the single largest finding of planets to date.

Kepler data have also helped scientists observe and understand supernovae; measurements were collected every half-hour so the light curves were especially useful for studying these types of astronomical events.

On October 30, 2018, after the spacecraft ran out of fuel, NASA announced that the telescope would be retired. The telescope was shut down the same day, bringing an end to its nine-year service. Kepler observed 530,506 stars and discovered 2,662 exoplanets over its lifetime. A newer NASA mission, TESS, launched in 2018, is continuing the search for exoplanets.

Spacecraft design

The telescope has a mass of 1039 kg and contains a Schmidt camera with a 0.95 m front corrector plate (lens) feeding a 1.4 m primary mirror—at the time of its launch this was the largest mirror on any telescope outside Earth orbit, though the Herschel Space Observatory took this title a few months later. Its telescope has a 115 deg2 (about 12-degree diameter) field of view (FoV), roughly equivalent to the size of one's fist held at arm's length. Of this, 105 deg2 is of science quality, with less than 11% vignetting. The photometer has a soft focus to provide excellent photometry, rather than sharp images. The mission goal was a combined differential photometric precision (CDPP) of 20 ppm for a m(V)=12 Sun-like star for a 6.5-hour integration, though the observations fell short of this objective (see mission status).

Camera

The focal plane of the spacecraft's camera is made out of forty-two 50 xx CCDs at 2200×1024 pixels each, possessing a total resolution of 94.6 megapixels, which at the time made it the largest camera system launched into space. The array was cooled by heat pipes connected to an external radiator. The CCDs were read out every 6.5 seconds (to limit saturation) and co-added on board for 58.89 seconds for short cadence targets, and 1765.5 seconds (29.4 minutes) for long cadence targets. Due to the larger bandwidth requirements for the former, these were limited in number to 512 compared to 170,000 for long cadence. However, even though at launch Kepler had the highest data rate of any NASA mission, the 29-minute sums of all 95 million pixels constituted more data than could be stored and sent back to Earth. Therefore, the science team pre-selected the relevant pixels associated with each star of interest, amounting to about 6 percent of the pixels (5.4 megapixels). The data from these pixels was then requantized, compressed and stored, along with other auxiliary data, in the on-board 16 gigabyte solid-state recorder. Data that was stored and downlinked includes science stars, p-mode stars, smear, black level, background and full field-of-view images.

Primary mirror

The Kepler primary mirror is 1.4 m in diameter. Manufactured by glass maker Corning using ultra-low expansion (ULE) glass, the mirror is specifically designed to have a mass only 14% that of a solid mirror of the same size. To produce a space telescope system with sufficient sensitivity to detect relatively small planets, as they pass in front of stars, a very high reflectance coating on the primary mirror was required. Using ion assisted evaporation, Surface Optics Corp. applied a protective nine-layer silver coating to enhance reflection and a dielectric interference coating to minimize the formation of color centers and atmospheric moisture absorption.

Photometric performance
In terms of photometric performance, Kepler worked well, much better than any Earth-bound telescope, but short of design goals. The objective was a combined differential photometric precision (CDPP) of 20 parts per million (PPM) on a magnitude 12 star for a 6.5-hour integration. This estimate was developed allowing 10 ppm for stellar variability, roughly the value for the Sun. The obtained accuracy for this observation has a wide range, depending on the star and position on the focal plane, with a median of 29 ppm. Most of the additional noise appears to be due to a larger-than-expected variability in the stars themselves (19.5 ppm as opposed to the assumed 10.0 ppm), with the rest due to instrumental noise sources slightly larger than predicted.

Because decrease in brightness from an Earth-size planet transiting a Sun-like star is so small, only 80 ppm, the increased noise means each individual transit is only a 2.7 σ event, instead of the intended 4 σ. This, in turn, means more transits must be observed to be sure of a detection. Scientific estimates indicated that a mission lasting 7 to 8 years, as opposed to the originally planned 3.5 years, would be needed to find all transiting Earth-sized planets. On April 4, 2012, the Kepler mission was approved for extension through the fiscal year 2016, but this also depended on all remaining reaction wheels staying healthy, which turned out not to be the case (see Reaction wheel issues below).

Orbit and orientation
Kepler orbits the Sun, which avoids Earth occultations, stray light, and gravitational perturbations and torques inherent in an Earth orbit.

NASA has characterized Kepler's orbit as "Earth-trailing". With an orbital period of 372.5 days, Kepler is slowly falling farther behind Earth (about 16 million miles per annum). , the distance to Kepler from Earth was about 0.917 AU. This means that after about 26 years Kepler will reach the other side of the Sun and will get back to the neighborhood of the Earth after 51 years.

Until 2013 the photometer pointed to a field in the northern constellations of Cygnus, Lyra and Draco, which is well out of the ecliptic plane, so that sunlight never enters the photometer as the spacecraft orbits. This is also the direction of the Solar System's motion around the center of the galaxy. Thus, the stars which Kepler observed are roughly the same distance from the Galactic Center as the Solar System, and also close to the galactic plane. This fact is important if position in the galaxy is related to habitability, as suggested by the Rare Earth hypothesis.

Orientation is three-axis stabilized by sensing rotations using fine-guidance sensors located on the instrument focal plane (instead of rate sensing gyroscopes, e.g. as used on Hubble). and using reaction wheels and hydrazine thrusters to control the orientation.

Operations

Kepler was operated out of Boulder, Colorado, by the Laboratory for Atmospheric and Space Physics (LASP) under contract to Ball Aerospace & Technologies. The spacecraft's solar array was rotated to face the Sun at the solstices and equinoxes, so as to optimize the amount of sunlight falling on the solar array and to keep the heat radiator pointing towards deep space. Together, LASP and Ball Aerospace controlled the spacecraft from a mission operations center located on the research campus of the University of Colorado. LASP performs essential mission planning and the initial collection and distribution of the science data. The mission's initial life-cycle cost was estimated at US$600 million, including funding for 3.5 years of operation. In 2012, NASA announced that the Kepler mission would be funded until 2016 at a cost of about $20 million per year.

Communications
NASA contacted the spacecraft using the X band communication link twice a week for command and status updates. Scientific data are downloaded once a month using the Ka band link at a maximum data transfer rate of approximately 550 kB/s. The high gain antenna is not steerable so data collection is interrupted for a day to reorient the whole spacecraft and the high gain antenna for communications to Earth.

The Kepler space telescope conducted its own partial analysis on board and only transmitted scientific data deemed necessary to the mission in order to conserve bandwidth.

Data management
Science data telemetry collected during mission operations at LASP is sent for processing to the Kepler Data Management Center (DMC) which is located at the Space Telescope Science Institute on the campus of Johns Hopkins University in Baltimore, Maryland. The science data telemetry is decoded and processed into uncalibrated FITS-format science data products by the DMC, which are then passed along to the Science Operations Center (SOC) at NASA Ames Research Center, for calibration and final processing. The SOC at NASA Ames Research Center (ARC) develops and operates the tools needed to process scientific data for use by the Kepler Science Office (SO). Accordingly, the SOC develops the pipeline data processing software based on scientific algorithms developed jointly by the SO and SOC. During operations, the SOC: The SOC also evaluates the photometric performance on an ongoing basis and provides the performance metrics to the SO and Mission Management Office. Finally, the SOC develops and maintains the project's scientific databases, including catalogs and processed data. The SOC finally returns calibrated data products and scientific results back to the DMC for long-term archiving, and distribution to astronomers around the world through the Multimission Archive at STScI (MAST).
 * 1) Receives uncalibrated pixel data from the DMC
 * 2) Applies the analysis algorithms to produce calibrated pixels and light curves for each star
 * 3) Performs transit searches for detection of planets (threshold-crossing events, or TCEs)
 * 4) Performs data validation of candidate planets by evaluating various data products for consistency as a way to eliminate false positive detections

Reaction wheel failures
On July 14, 2012, one of the four reaction wheels used for fine pointing of the spacecraft failed. While Kepler requires only three reaction wheels to accurately aim the telescope, another failure would leave the spacecraft unable to aim at its original field.

After showing some problems in January 2013, a second reaction wheel failed on May 11, 2013, ending Kepler's primary mission. The spacecraft was put into safe mode, then from June to August 2013 a series of engineering tests were done to try to recover either failed wheel. By August 15, 2013, it was decided that the wheels were unrecoverable,  and an engineering report was ordered to assess the spacecraft's remaining capabilities.

This effort ultimately led to the "K2" follow-on mission observing different fields near the ecliptic.

Operational timeline

In January 2006, the project's launch was delayed eight months because of budget cuts and consolidation at NASA. It was delayed again by four months in March 2006 due to fiscal problems. At this time, the high-gain antenna was changed from a gimballed design to one fixed to the frame of the spacecraft to reduce cost and complexity, at the cost of one observation day per month.

The Kepler observatory was launched on March 7, 2009, at 03:49:57 UTC aboard a Delta II rocket from Cape Canaveral Air Force Station, Florida. The launch was a success and all three stages were completed by 04:55 UTC. The cover of the telescope was jettisoned on April 7, 2009, and the first light images were taken on the next day.

On April 20, 2009, it was announced that the Kepler science team had concluded that further refinement of the focus would dramatically increase the scientific return. On April 23, 2009, it was announced that the focus had been successfully optimized by moving the primary mirror 40 micrometers (1.6 thousandths of an inch) towards the focal plane and tilting the primary mirror 0.0072 degree.

On May 13, 2009, at 00:01 UTC, Kepler successfully completed its commissioning phase and began its search for planets around other stars.

On June 19, 2009, the spacecraft successfully sent its first science data to Earth. It was discovered that Kepler had entered safe mode on June 15. A second safe mode event occurred on July 2. In both cases the event was triggered by a processor reset. The spacecraft resumed normal operation on July 3 and the science data that had been collected since June 19 was downlinked that day. On October 14, 2009, the cause of these safing events was determined to be a low voltage power supply that provides power to the RAD750 processor. On January 12, 2010, one portion of the focal plane transmitted anomalous data, suggesting a problem with focal plane MOD-3 module, covering two out of Kepler's 42 CCDs. , the module was described as "failed", but the coverage still exceeded the science goals.

Kepler downlinked roughly twelve gigabytes of data about once per month.

Field of view
Kepler has a fixed field of view (FOV) against the sky. The diagram to the right shows the celestial coordinates and where the detector fields are located, along with the locations of a few bright stars with celestial north at the top left corner. The mission website has a calculator that will determine if a given object falls in the FOV, and if so, where it will appear in the photo detector output data stream. Data on exoplanet candidates is submitted to the Kepler Follow-up Program, or KFOP, to conduct follow-up observations.

Kepler's field of view covers 115 square degrees, around 0.25 percent of the sky, or "about two scoops of the Big Dipper". Thus, it would require around 400 Kepler-like telescopes to cover the whole sky. The Kepler field contains portions of the constellations Cygnus, Lyra, and Draco.

The nearest star system in Kepler's field of view is the trinary star system Gliese 1245, 15 light years from the Sun. The brown dwarf WISE J2000+3629, 22.8 ± 1 light years from the Sun is also in the field of view, but is invisible to Kepler due to emitting light primarily in infrared wavelengths.

Objectives and methods
The scientific objective of the Kepler space telescope was to explore the structure and diversity of planetary systems. This spacecraft observes a large sample of stars to achieve several key goals:

 * To determine how many Earth-size and larger planets there are in or near the habitable zone (often called "Goldilocks planets") of a wide variety of spectral types of stars.
 * To determine the range of size and shape of the orbits of these planets.
 * To estimate how many planets there are in multiple-star systems.
 * To determine the range of orbit size, brightness, size, mass and density of short-period giant planets.
 * To identify additional members of each discovered planetary system using other techniques.
 * Determine the properties of those stars that harbor planetary systems.

Most of the exoplanets previously detected by other projects were giant planets, mostly the size of Jupiter and bigger. Kepler was designed to look for planets 30 to 600 times less massive, closer to the order of Earth's mass (Jupiter is 318 times more massive than Earth). The method used, the transit method, involves observing repeated transit of planets in front of their stars, which causes a slight reduction in the star's apparent magnitude, on the order of 0.01% for an Earth-size planet. The degree of this reduction in brightness can be used to deduce the diameter of the planet, and the interval between transits can be used to deduce the planet's orbital period, from which estimates of its orbital semi-major axis (using Kepler's laws) and its temperature (using models of stellar radiation) can be calculated.

The probability of a random planetary orbit being along the line-of-sight to a star is the diameter of the star divided by the diameter of the orbit. For an Earth-size planet at 1 AU transiting a Sun-like star the probability is 0.47%, or about 1 in 210. For a planet like Venus orbiting a Sun-like star the probability is slightly higher, at 0.65%; If the host star has multiple planets, the probability of additional detections is higher than the probability of initial detection assuming planets in a given system tend to orbit in similar planes—an assumption consistent with current models of planetary system formation. For instance, if a Kepler-like mission conducted by aliens observed Earth transiting the Sun, there is a 7% chance that it would also see Venus transiting.

Kepler's 115 deg2 field of view gives it a much higher probability of detecting Earth-sized planets than the Hubble Space Telescope, which has a field of view of only 10 sq. arc-minutes. Moreover, Kepler is dedicated to detecting planetary transits, while the Hubble Space Telescope is used to address a wide range of scientific questions, and rarely looks continuously at just one starfield. Of the approximately half-million stars in Kepler's field of view, around 150,000 stars were selected for observation. More than 90,000 are G-type stars on, or near, the main sequence. Thus, Kepler was designed to be sensitive to wavelengths of 400–865 nm where brightness of those stars peaks. Most of the stars observed by Kepler have apparent visual magnitude between 14 and 16 but the brightest observed stars have apparent visual magnitude of 8 or lower. Most of the planet candidates were initially not expected to be confirmed due to being too faint for follow-up observations. All the selected stars are observed simultaneously, with the spacecraft measuring variations in their brightness every thirty minutes. This provides a better chance for seeing a transit. The mission was designed to maximize the probability of detecting planets orbiting other stars.

Because Kepler must observe at least three transits to confirm that the dimming of a star was caused by a transiting planet, and because larger planets give a signal that is easier to check, scientists expected the first reported results to be larger Jupiter-size planets in tight orbits. The first of these were reported after only a few months of operation. Smaller planets, and planets farther from their sun would take longer, and discovering planets comparable to Earth were expected to take three years or longer.

Data collected by Kepler is also being used for studying variable stars of various types and performing asteroseismology, particularly on stars showing solar-like oscillations.

Finding planet candidates

Once Kepler has collected and sent back the data, raw light curves are constructed. Brightness values are then adjusted to take the brightness variations due to the rotation of the spacecraft into account. The next step is processing (folding) light curves into a more easily observable form and letting software select signals that seem potentially transit-like. At this point, any signal that shows potential transit-like features is called a threshold crossing event. These signals are individually inspected in two inspection rounds, with the first round taking only a few seconds per target. This inspection eliminates erroneously selected non-signals, signals caused by instrumental noise and obvious eclipsing binaries.

Threshold crossing events that pass these tests are called Kepler Objects of Interest (KOI), receive a KOI designation and are archived. KOIs are inspected more thoroughly in a process called dispositioning. Those which pass the dispositioning are called Kepler planet candidates. The KOI archive is not static, meaning that a Kepler candidate could end up in the false-positive list upon further inspection. In turn, KOIs that were mistakenly classified as false positives could end up back in the candidates list.

Not all the planet candidates go through this process. Circumbinary planets do not show strictly periodic transits, and have to be inspected through other methods. In addition, third-party researchers use different data-processing methods, or even search planet candidates from the unprocessed light curve data. As a consequence, those planets may be missing KOI designation.

Confirming planet candidates
Once suitable candidates have been found from Kepler data, it is necessary to rule out false positives with follow-up tests.

Usually, Kepler candidates are imaged individually with more-advanced ground-based telescopes in order to resolve any background objects which could contaminate the brightness signature of the transit signal. Another method to rule out planet candidates is astrometry for which Kepler can collect good data even though doing so was not a design goal. While Kepler cannot detect planetary-mass objects with this method, it can be used to determine if the transit was caused by a stellar-mass object.

Through other detection methods
There are a few different exoplanet detection methods which help to rule out false positives by giving further proof that a candidate is a real planet. One of the methods, called doppler spectroscopy, requires follow-up observations from ground-based telescopes. This method works well if the planet is massive or is located around a relatively bright star. While current spectrographs are insufficient for confirming planetary candidates with small masses around relatively dim stars, this method can be used to discover additional massive non-transiting planet candidates around targeted stars.

In multiplanetary systems, planets can often be confirmed through transit timing variation by looking at the time between successive transits, which may vary if planets are gravitationally perturbed by each other. This helps to confirm relatively low-mass planets even when the star is relatively distant. Transit timing variations indicate that two or more planets belong to the same planetary system. There are even cases where a non-transiting planet is also discovered in this way.

Circumbinary planets show much larger transit timing variations between transits than planets gravitationally disturbed by other planets. Their transit duration times also vary significantly. Transit timing and duration variations for circumbinary planets are caused by the orbital motion of the host stars, rather than by other planets. In addition, if the planet is massive enough, it can cause slight variations of the host stars' orbital periods. Despite being harder to find circumbinary planets due to their non-periodic transits, it is much easier to confirm them, as timing patterns of transits cannot be mimicked by an eclipsing binary or a background star system.

In addition to transits, planets orbiting around their stars undergo reflected-light variations—like the Moon, they go through phases from full to new and back again. Because Kepler cannot resolve the planet from the star, it sees only the combined light, and the brightness of the host star seems to change over each orbit in a periodic manner. Although the effect is small—the photometric precision required to see a close-in giant planet is about the same as to detect an Earth-sized planet in transit across a solar-type star—Jupiter-sized planets with an orbital period of a few days or less are detectable by sensitive space telescopes such as Kepler. In the long run, this method may help find more planets than the transit method, because the reflected light variation with orbital phase is largely independent of the planet's orbital inclination, and does not require the planet to pass in front of the disk of the star. In addition, the phase function of a giant planet is also a function of its thermal properties and atmosphere, if any. Therefore, the phase curve may constrain other planetary properties, such as the particle size distribution of the atmospheric particles.

Kepler's photometric precision is often high enough to observe a star's brightness changes caused by doppler beaming or a star's shape deformation by a companion. These can sometimes be used to rule out hot Jupiter candidates as false positives caused by a star or a brown dwarf when these effects are too noticeable. However, there are some cases where such effects are detected even by planetary-mass companions such as TrES-2b.

Through validation
If a planet cannot be detected through at least one of the other detection methods, it can be confirmed by determining if the possibility of a Kepler candidate being a real planet is significantly larger than any false-positive scenarios combined. One of the first methods was to see if other telescopes can see the transit as well. The first planet confirmed through this method was Kepler-22b which was also observed with the Spitzer Space Telescope in addition to analyzing any other false-positive possibilities. Such confirmation is costly, as small planets can generally be detected only with space telescopes.

In 2014, a new confirmation method called "validation by multiplicity" was announced. From the planets previously confirmed through various methods, it was found that planets in most planetary systems orbit in a relatively flat plane, similar to the planets found in the Solar System. This means that if a star has multiple planet candidates, it is very likely a real planetary system. Transit signals still need to meet several criteria which rule out false-positive scenarios. For instance, it has to have considerable signal-to-noise ratio, it has at least three observed transits, orbital stability of those systems have to be stable and transit curve has to have a shape that partly eclipsing binaries could not mimic the transit signal. In addition, its orbital period needs to be 1.6 days or longer to rule out common false positives caused by eclipsing binaries. Validation by multiplicity method is very efficient and allows to confirm hundreds of Kepler candidates in a relatively short amount of time.

A new validation method using a tool called PASTIS has been developed. It makes it possible to confirm a planet even when only a single candidate transit event for the host star has been detected. A drawback of this tool is that it requires a relatively high signal-to-noise ratio from Kepler data, so it can mainly confirm only larger planets or planets around quiet and relatively bright stars. Currently, the analysis of Kepler candidates through this method is underway. PASTIS was first successful for validating the planet Kepler-420b.

K2 Extension

In April 2012, an independent panel of senior NASA scientists recommended that the Kepler mission be continued through 2016. According to the senior review, Kepler observations needed to continue until at least 2015 to achieve all the stated scientific goals. On November 14, 2012, NASA announced the completion of Kepler's primary mission, and the beginning of its extended mission, which ended in 2018 when it ran out of fuel.

Reaction wheel issues
In July 2012, one of Kepler's four reaction wheels (wheel 2) failed. On May 11, 2013, a second wheel (wheel 4) failed, jeopardizing the continuation of the mission, as three wheels are necessary for its planet hunting. Kepler had not collected science data since May because it was not able to point with sufficient accuracy. On July 18 and 22 reaction wheels 4 and 2 were tested respectively; wheel 4 only rotated counter-clockwise but wheel 2 ran in both directions, albeit with significantly elevated friction levels. A further test of wheel 4 on July 25 managed to achieve bi-directional rotation. Both wheels, however, exhibited too much friction to be useful. On August 2, NASA put out a call for proposals to use the remaining capabilities of Kepler for other scientific missions. Starting on August 8, a full systems evaluation was conducted. It was determined that wheel 2 could not provide sufficient precision for scientific missions and the spacecraft was returned to a "rest" state to conserve fuel. Wheel 4 was previously ruled out because it exhibited higher friction levels than wheel 2 in previous tests. Sending astronauts to fix Kepler is not an option because it orbits the Sun and is millions of kilometers from Earth.

On August 15, 2013, NASA announced that Kepler would not continue searching for planets using the transit method after attempts to resolve issues with two of the four reaction wheels failed. An engineering report was ordered to assess the spacecraft's capabilities, its two good reaction wheels and its thrusters. Concurrently, a scientific study was conducted to determine whether enough knowledge can be obtained from Kepler's limited scope to justify its $18 million per year cost.

Possible ideas included searching for asteroids and comets, looking for evidence of supernovas, and finding huge exoplanets through gravitational microlensing. Another proposal was to modify the software on Kepler to compensate for the disabled reaction wheels. Instead of the stars being fixed and stable in Kepler's field of view, they will drift. Proposed software was to track this drift and more or less completely recover the mission goals despite being unable to hold the stars in a fixed view.

Previously collected data continued to be analyzed.

Second Light (K2)
In November 2013, a new mission plan named K2 "Second Light" was presented for consideration. K2 would involve using Kepler's remaining capability, photometric precision of about 300 parts per million, compared with about 20 parts per million earlier, to collect data for the study of "supernova explosions, star formation and Solar-System bodies such as asteroids and comets, ... " and for finding and studying more exoplanets. In this proposed mission plan, Kepler would search a much larger area in the plane of Earth's orbit around the Sun. Celestial objects, including exoplanets, stars and others, detected by the K2 mission would be associated with the EPIC acronym, standing for Ecliptic Plane Input Catalog.

In early 2014, the spacecraft underwent successful testing for the K2 mission. From March to May 2014, data from a new field called Field 0 was collected as a testing run. On May 16, 2014, NASA announced the approval of extending the Kepler mission to the K2 mission. Kepler's photometric precision for the K2 mission was estimated to be 50 ppm on a magnitude 12 star for a 6.5-hour integration. In February 2014, photometric precision for the K2 mission using two-wheel, fine-point precision operations was measured as 44 ppm on magnitude 12 stars for a 6.5-hour integration. The analysis of these measurements by NASA suggests the K2 photometric precision approaches that of the Kepler archive of three-wheel, fine-point precision data.

On May 29, 2014, campaign fields 0 to 13 were reported and described in detail. Field 1 of the K2 mission is set towards the Leo-Virgo region of the sky, while Field 2 is towards the "head" area of Scorpius and includes two globular clusters, Messier 4 and Messier 80, and part of the Scorpius–Centaurus association, which is only about 11 million years old and 380 - 470 ly distant with probably over 1,000 members.

On December 18, 2014, NASA announced that the K2 mission had detected its first confirmed exoplanet, a super-Earth named HIP 116454 b. Its signature was found in a set of engineering data meant to prepare the spacecraft for the full K2 mission. Radial velocity follow-up observations were needed as only a single transit of the planet was detected.

During a scheduled contact on April 7, 2016, Kepler was found to be operating in emergency mode, the lowest operational and most fuel intensive mode. Mission operations declared a spacecraft emergency, which afforded them priority access to NASA's Deep Space Network. By the evening of April 8 the spacecraft had been upgraded to safe mode, and on April 10 it was placed into point-rest state, a stable mode which provides normal communication and the lowest fuel burn. At that time, the cause of the emergency was unknown, but it was not believed that Kepler's reaction wheels or a planned maneuver to support K2 Campaign 9 were responsible. Operators downloaded and analyzed engineering data from the spacecraft, with the prioritization of returning to normal science operations. Kepler was returned to science mode on April 22. The emergency caused the first half of Campaign 9 to be shortened by two weeks.

In June 2016, NASA announced a K2 mission extension of three additional years, beyond the expected exhaustion of on-board fuel in 2018. In August 2018, NASA roused the spacecraft from sleep mode, applied a modified configuration to deal with thruster problems that degraded pointing performance, and began collecting scientific data for the 19th observation campaign, finding that the onboard fuel was not yet utterly exhausted.

On October 30, 2018, NASA announced that the spacecraft was out of fuel and its mission was officially ended.

Mission results

The Kepler space telescope was in active operation from 2009 through 2013, with the first main results announced on January 4, 2010. As expected, the initial discoveries were all short-period planets. As the mission continued, additional longer-period candidates were found. , Kepler has discovered 5,011 exoplanet candidates and 2,662 confirmed exoplanets. As of August 2022, 2,056 exoplanet candidates remain to be confirmed and 2,711 are now confirmed exoplanets.

2009
NASA held a press conference to discuss early science results of the Kepler mission on August 6, 2009. At this press conference, it was revealed that Kepler had confirmed the existence of the previously known transiting exoplanet HAT-P-7b, and was functioning well enough to discover Earth-size planets.

Because Kepler's detection of planets depends on seeing very small changes in brightness, stars that vary in brightness by themselves (variable stars) are not useful in this search. From the first few months of data, Kepler scientists determined that about 7,500 stars from the initial target list are such variable stars. These were dropped from the target list, and replaced by new candidates. On November 4, 2009, the Kepler project publicly released the light curves of the dropped stars. The first new planet candidate observed by Kepler was originally marked as a false positive because of uncertainties in the mass of its parent star. However, it was confirmed ten years later and is now designated Kepler-1658b.

The first six weeks of data revealed five previously unknown planets, all very close to their stars. Among the notable results are one of the least dense planets yet found, two low-mass white dwarfs that were initially reported as being members of a new class of stellar objects, and Kepler-16b, a well-characterized planet orbiting a binary star.

2010
On June 15, 2010, the Kepler mission released data on all but 400 of the ~156,000 planetary target stars to the public. 706 targets from this first data set have viable exoplanet candidates, with sizes ranging from as small as Earth to larger than Jupiter. The identity and characteristics of 306 of the 706 targets were given. The released targets included five candidate multi-planet systems, including six extra exoplanet candidates. Only 33.5 days of data were available for most of the candidates. NASA also announced data for another 400 candidates were being withheld to allow members of the Kepler team to perform follow-up observations. The data for these candidates was published February 2, 2011. (See the Kepler results for 2011 below.)

The Kepler results, based on the candidates in the list released in 2010, implied that most candidate planets have radii less than half that of Jupiter. The results also imply that small candidate planets with periods less than thirty days are much more common than large candidate planets with periods less than thirty days and that the ground-based discoveries are sampling the large-size tail of the size distribution. This contradicted older theories which had suggested small and Earth-size planets would be relatively infrequent. Based on extrapolations from the Kepler data, an estimate of around 100 million habitable planets in the Milky Way may be realistic. Some media reports of the TED talk have led to the misunderstanding that Kepler had actually found these planets. This was clarified in a letter to the Director of the NASA Ames Research Center, for the Kepler Science Council dated August 2, 2010 states, "Analysis of the current Kepler data does not support the assertion that Kepler has found any Earth-like planets."

In 2010, Kepler identified two systems containing objects which are smaller and hotter than their parent stars: KOI 74 and KOI 81. These objects are probably low-mass white dwarfs produced by previous episodes of mass transfer in their systems.

2011

On February 2, 2011, the Kepler team announced the results of analysis of the data taken between 2 May and September 16, 2009. They found 1235 planetary candidates circling 997 host stars. (The numbers that follow assume the candidates are really planets, though the official papers called them only candidates. Independent analysis indicated that at least 90% of them are real planets and not false positives). 68 planets were approximately Earth-size, 288 super-Earth-size, 662 Neptune-size, 165 Jupiter-size, and 19 up to twice the size of Jupiter. In contrast to previous work, roughly 74% of the planets are smaller than Neptune, most likely as a result of previous work finding large planets more easily than smaller ones.

That February 2, 2011 release of 1235 exoplanet candidates included 54 that may be in the "habitable zone", including five less than twice the size of Earth. There were previously only two planets thought to be in the "habitable zone", so these new findings represent an enormous expansion of the potential number of "Goldilocks planets" (planets of the right temperature to support liquid water). All of the habitable zone candidates found thus far orbit stars significantly smaller and cooler than the Sun (habitable candidates around Sun-like stars will take several additional years to accumulate the three transits required for detection). Of all the new planet candidates, 68 are 125% of Earth's size or smaller, or smaller than all previously discovered exoplanets. "Earth-size" and "super-Earth-size" is defined as "less than or equal to 2 Earth radii (Re)" [(or, Rp ≤ 2.0 Re) – Table 5]. Six such planet candidates [namely: KOI 326.01 (Rp=0.85), KOI 701.03 (Rp=1.73), KOI 268.01 (Rp=1.75), KOI 1026.01 (Rp=1.77), KOI 854.01 (Rp=1.91), KOI 70.03 (Rp=1.96) – Table 6] are in the "habitable zone." A more recent study found that one of these candidates (KOI 326.01) is in fact much larger and hotter than first reported.

The frequency of planet observations was highest for exoplanets two to three times Earth-size, and then declined in inverse proportionality to the area of the planet. The best estimate (as of March 2011), after accounting for observational biases, was: 5.4% of stars host Earth-size candidates, 6.8% host super-Earth-size candidates, 19.3% host Neptune-size candidates, and 2.55% host Jupiter-size or larger candidates. Multi-planet systems are common; 17% of the host stars have multi-candidate systems, and 33.9% of all the planets are in multiple planet systems.

By December 5, 2011, the Kepler team announced that they had discovered 2,326 planetary candidates, of which 207 are similar in size to Earth, 680 are super-Earth-size, 1,181 are Neptune-size, 203 are Jupiter-size and 55 are larger than Jupiter. Compared to the February 2011 figures, the number of Earth-size and super-Earth-size planets increased by 200% and 140% respectively. Moreover, 48 planet candidates were found in the habitable zones of surveyed stars, marking a decrease from the February figure; this was due to the more stringent criteria in use in the December data.

On December 20, 2011, the Kepler team announced the discovery of the first Earth-size exoplanets, Kepler-20e and Kepler-20f, orbiting a Sun-like star, Kepler-20.

Based on Kepler's findings, astronomer Seth Shostak estimated in 2011 that "within a thousand light-years of Earth", there are "at least 30,000" habitable planets. Also based on the findings, the Kepler team has estimated that there are "at least 50 billion planets in the Milky Way", of which "at least 500 million" are in the habitable zone. In March 2011, astronomers at NASA's Jet Propulsion Laboratory (JPL) reported that about "1.4 to 2.7 percent" of all Sun-like stars are expected to have Earth-size planets "within the habitable zones of their stars". This means there are "two billion" of these "Earth analogs" in the Milky Way alone. The JPL astronomers also noted that there are "50 billion other galaxies", potentially yielding more than one sextillion "Earth analog" planets if all galaxies have similar numbers of planets to the Milky Way.

2012
In January 2012, an international team of astronomers reported that each star in the Milky Way may host "on average...at least 1.6 planets", suggesting that over 160 billion star-bound planets may exist in the Milky Way. Kepler also recorded distant stellar super-flares, some of which are 10,000 times more powerful than the 1859 Carrington event. The superflares may be triggered by close-orbiting Jupiter-sized planets. The Transit Timing Variation (TTV) technique, which was used to discover Kepler-9d, gained popularity for confirming exoplanet discoveries. A planet in a system with four stars was also confirmed, the first time such a system had been discovered.

, there were a total of 2,321 candidates. Of these, 207 are similar in size to Earth, 680 are super-Earth-size, 1,181 are Neptune-size, 203 are Jupiter-size and 55 are larger than Jupiter. Moreover, 48 planet candidates were found in the habitable zones of surveyed stars. The Kepler team estimated that 5.4% of all stars host Earth-size planet candidates, and that 17% of all stars have multiple planets.

2013

According to a study by Caltech astronomers published in January 2013, the Milky Way contains at least as many planets as it does stars, resulting in 100–400 billion exoplanets. The study, based on planets orbiting the star Kepler-32, suggests that planetary systems may be common around stars in the Milky Way. The discovery of 461 more candidates was announced on January 7, 2013. The longer Kepler watches, the more planets with long periods it can detect.

Since the last Kepler catalog was released in February 2012, the number of candidates discovered in the Kepler data has increased by 20 percent and now totals 2,740 potential planets orbiting 2,036 stars

A candidate, newly announced on January 7, 2013, was Kepler-69c (formerly, KOI-172.02), an Earth-size exoplanet orbiting a star similar to the Sun in the habitable zone and possibly habitable.

In April 2013, a white dwarf was discovered bending the light of its companion red dwarf in the KOI-256 star system.

In April 2013, NASA announced the discovery of three new Earth-size exoplanets—Kepler-62e, Kepler-62f, and Kepler-69c—in the habitable zones of their respective host stars, Kepler-62 and Kepler-69. The new exoplanets are considered prime candidates for possessing liquid water and thus a habitable environment. A more recent analysis has shown that Kepler-69c is likely more analogous to Venus, and thus unlikely to be habitable.

On May 15, 2013, NASA announced the space telescope had been crippled by failure of a reaction wheel that keeps it pointed in the right direction. A second wheel had previously failed, and the telescope required three wheels (out of four total) to be operational for the instrument to function properly. Further testing in July and August determined that while Kepler was capable of using its damaged reaction wheels to prevent itself from entering safe mode and of downlinking previously collected science data it was not capable of collecting further science data as previously configured. Scientists working on the Kepler project said there was a backlog of data still to be looked at, and that more discoveries would be made in the following couple of years, despite the setback.

Although no new science data from Kepler field had been collected since the problem, an additional sixty-three candidates were announced in July 2013 based on the previously collected observations.

In November 2013, the second Kepler science conference was held. The discoveries included the median size of planet candidates getting smaller compared to early 2013, preliminary results of the discovery of a few circumbinary planets and planets in the habitable zone.

2014

On February 13, over 530 additional planet candidates were announced residing around single planet systems. Several of them were nearly Earth-sized and located in the habitable zone. This number was further increased by about 400 in June 2014.

On February 26, scientists announced that data from Kepler had confirmed the existence of 715 new exoplanets. A new statistical method of confirmation was used called "verification by multiplicity" which is based on how many planets around multiple stars were found to be real planets. This allowed much quicker confirmation of numerous candidates which are part of multiplanetary systems. 95% of the discovered exoplanets were smaller than Neptune and four, including Kepler-296f, were less than 2 1/2 the size of Earth and were in habitable zones where surface temperatures are suitable for liquid water.

In March, a study found that small planets with orbital periods of less than one day are usually accompanied by at least one additional planet with orbital period of 1–50 days. This study also noted that ultra-short period planets are almost always smaller than 2 Earth radii unless it is a misaligned hot Jupiter.

On April 17, the Kepler team announced the discovery of Kepler-186f, the first nearly Earth-sized planet located in the habitable zone. This planet orbits around a red dwarf.

In May 2014, K2 observations fields 0 to 13 were announced and described in detail. K2 observations began in June 2014.

In July 2014, the first discoveries from K2 field data were reported in the form of eclipsing binaries. Discoveries were derived from a Kepler engineering data set which was collected prior to campaign 0 in preparation to the main K2 mission.

On September 23, 2014, NASA reported that the K2 mission had completed campaign 1, the first official set of science observations, and that campaign 2 was underway.

Campaign 3 lasted from November 14, 2014, to February 6, 2015, and included "16,375 standard long cadence and 55 standard short cadence targets".

2015

 * In January 2015, the number of confirmed Kepler planets exceeded 1000. At least two (Kepler-438b and Kepler-442b) of the discovered planets announced that month were likely rocky and in the habitable zone. Also in January 2015, NASA reported that five confirmed sub-earth-sized rocky exoplanets, all smaller than the planet Venus, were found orbiting the 11.2 billion year old star Kepler-444, making this star system, at 80% of the age of the universe, the oldest yet discovered.
 * In April 2015, campaign 4 was reported to last between February 7, 2015, and April 24, 2015, and to include observations of nearly 16,000 target stars and two notable open star clusters, Pleiades and Hyades.
 * In May 2015, Kepler observed a newly discovered supernova, KSN 2011b (Type 1a), before, during and after explosion. Details of the pre-nova moments may help scientists better understand dark energy.
 * On July 24, 2015, NASA announced the discovery of Kepler-452b, a confirmed exoplanet that is near-Earth in size and found orbiting the habitable zone of a Sun-like star. The seventh Kepler planet candidate catalog was released, containing 4,696 candidates, and increase of 521 candidates since the previous catalog release in January 2015.
 * On September 14, 2015, astronomers reported unusual light fluctuations of KIC 8462852, an F-type main-sequence star in the constellation Cygnus, as detected by Kepler, while searching for exoplanets. Various hypotheses have been presented, including comets, asteroids, and an alien civilization.

2016
By May 10, 2016, the Kepler mission had verified 1,284 new planets. Based on their size, about 550 could be rocky planets. Nine of these orbit in their stars' habitable zone: Kepler-560b, Kepler-705b, Kepler-1229b, Kepler-1410b, Kepler-1455b, Kepler-1544 b, Kepler-1593b, Kepler-1606b, and Kepler-1638b.

Data releases
The Kepler team originally promised to release data within one year of observations. However, this plan was changed after launch, with data being scheduled for release up to three years after its collection. This resulted in considerable criticism,    leading the Kepler science team to release the third quarter of their data one year and nine months after collection. The data through September 2010 (quarters 4, 5, and 6) was made public in January 2012.

Follow-ups by others
Periodically, the Kepler team releases a list of candidates (Kepler Objects of Interest, or KOIs) to the public. Using this information, a team of astronomers collected radial velocity data using the SOPHIE échelle spectrograph to confirm the existence of the candidate KOI-428b in 2010, later named Kepler-40b. In 2011, the same team confirmed candidate KOI-423b, later named Kepler-39b.

Citizen scientist participation
Since December 2010, Kepler mission data has been used for the Planet Hunters project, which allows volunteers to look for transit events in the light curves of Kepler images to identify planets that computer algorithms might miss. By June 2011, users had found sixty-nine potential candidates that were previously unrecognized by the Kepler mission team. The team has plans to publicly credit amateurs who spot such planets.

In January 2012, the BBC program Stargazing Live aired a public appeal for volunteers to analyse Planethunters.org data for potential new exoplanets. This led two amateur astronomers—one in Peterborough, England—to discover a new Neptune-sized exoplanet, to be named Threapleton Holmes B. One hundred thousand other volunteers were also engaged in the search by late January, analyzing over one million Kepler images by early 2012. One such exoplanet, PH1b (or Kepler-64b from its Kepler designation), was discovered in 2012. A second exoplanet, PH2b (Kepler-86b) was discovered in 2013.

In April 2017, ABC Stargazing Live, a variation of BBC Stargazing Live, launched the Zooniverse project "Exoplanet Explorers". While Planethunters.org worked with archived data, Exoplanet Explorers used recently downlinked data from the K2 mission. On the first day of the project, 184 transit candidates were identified that passed simple tests. On the second day, the research team identified a star system, later named K2-138, with a Sun-like star and four super-Earths in a tight orbit. In the end, volunteers helped to identify 90 exoplanet candidates. The citizen scientists that helped discover the new star system will be added as co-authors in the research paper when published.

Confirmed exoplanets

Exoplanets discovered using Kepler data, but confirmed by outside researchers, include Kepler-39b, Kepler-40b, Kepler-41b, Kepler-43b, Kepler-44b, Kepler-45b, as well as the planets orbiting Kepler-223 and Kepler-42. The "KOI" acronym indicates that the star is a Kepler Object of Interest.

Kepler Input Catalog
The Kepler Input Catalog is a publicly searchable database of roughly 13.2 million targets used for the Kepler Spectral Classification Program and the Kepler mission. The catalog alone is not used for finding Kepler targets, because only a portion of the listed stars (about one-third of the catalog) can be observed by the spacecraft.

Solar System observations
Kepler has been assigned an observatory code in order to report its astrometric observations of small Solar System bodies to the Minor Planet Center. In 2013 the alternative NEOKepler mission was proposed, a search for near-Earth objects, in particular potentially hazardous asteroids (PHAs). Its unique orbit and larger field of view than existing survey telescopes allow it to look for objects inside Earth's orbit. It was predicted a 12-month survey could make a significant contribution to the hunt for PHAs as well as potentially locating targets for NASA's Asteroid Redirect Mission. Kepler's first discovery in the Solar System, however, was, a 200-kilometer cold classical Kuiper belt object located beyond the orbit of Neptune.

Retirement
On October 30, 2018, NASA announced that the Kepler space telescope, having run out of fuel, and after nine years of service and the discovery of over 2,600 exoplanets, has been officially retired, and will maintain its current, safe orbit, away from Earth. The spacecraft was deactivated with a "goodnight" command sent from the mission's control center at the Laboratory for Atmospheric and Space Physics on November 15, 2018. Kepler's retirement coincides with the 388th anniversary of Johannes Kepler's death in 1630.

title: Kepler space telescope


text:
Kevin McClory

Kevin O'Donovan McClory (8 June 1924 – 20 November 2006) was an Irish screenwriter, film producer, and film director. McClory was best known for producing the James Bond film Thunderball and for his legal battles with the character's creator, Ian Fleming (later United Artists, Metro-Goldwyn-Mayer Pictures and Eon Productions).

Early years
McClory was born in Dún Laoghaire, County Dublin, in 1924, to noted actor Thomas John O'Donovan McClory (stage name Desmond O'Donovan) and Winifrede (née Doran), a writer, teacher and actress. He suffered from dyslexia. McClory's ancestry goes back to the famous Brontë family. Elinor McClory was the mother of Patrick Prunty who changed his name to Bronte when he emigrated from Ireland to England in 1802. Patrick was the father of Emily, Anne, Charlotte, and Branwell Brontë. McClory's parents were actors and theatre producers in Ireland.

Second World War
As a teenaged radio officer in the British Merchant Navy, McClory endured attacks by German U-boats on two different occasions. The first attack occurred on 20 September 1942 while he was serving aboard The Mathilda. A U-Boat surfaced and attacked the ship with heavy machine gun fire. The crew of the ship fired back, and the U-Boat retreated. The second attack occurred on 21 February 1943 when McClory was serving on the Norwegian tanker Stigstad, which was attacked by multiple U-boats when it was a part of Convoy ON 166. The ship sank, and McClory and the other survivors made it to a life raft. They survived in terrible conditions for two weeks and travelled more than 600 miles before being rescued off the coast of Ireland. Two seaman died on the raft, and a third died soon after they were rescued. McClory suffered severe frostbite and lost the ability to speak for more than a year after the incident. When he recovered his voice, he was left with a pronounced stammer. He served out the rest of the war in Britain's Royal Navy.

1950s
McClory started a career at Shepperton Studios in Middlesex as a film boom operator and location manager, where he worked on The Cockleshell Heroes for Warwick Films. He was an assistant to John Huston on films including The African Queen (1951) and Moulin Rouge (1952). He was an assistant director on Huston's version of Moby-Dick (1956), and associate producer and second-unit director on Mike Todd's Around the World in 80 Days (also 1956).

McClory was romantically involved with Elizabeth Taylor. Although he and Taylor reportedly had plans to marry, she eventually left him for her future husband Mike Todd. Todd and McClory fell out over Taylor, yet they managed to complete the final cut of the film side by side. The trio would eventually reconcile, and they remained friends until Todd's untimely death in 1958.

In 1957, McClory led an expedition of 25 men in an attempt to drive around the world. He filmed a documentary of the adventure, One Road, as well as a series of ads for his sponsor Ford Motor Company. The team completed the journey in 104 days. He later wrote, produced and directed the 1957 film The Boy and the Bridge, with financial assistance from heiress Josephine Hartford Bryce (sister of Huntington Hartford) and her husband Ivor Bryce, a friend of Ian Fleming.

1960s
In 1958 Fleming approached McClory to produce the first Bond film. McClory rejected all of Fleming's books but felt that the character James Bond could be adapted for the screen. McClory, Bryce, Fleming and Jack Whittingham developed the character through a number of treatments and screenplays. McClory, Fleming and Bryce settled on a screenplay, Longitude 78 West (later renamed Thunderball), and went into pre-production. Fleming novelised the draft screenplay as his ninth novel,Thunderball, in 1961 and initially did not credit McClory or Whittingham. McClory and Whittingham engaged libel lawyer Peter Carter-Ruck and sued Fleming shortly after the 1961 publication of the Thunderball novel, claiming he based it upon the screenplay the trio had earlier written.

The trial opened in the High Court in London on 20 November 1963. After nine days, the case was settled out of court. Fleming paid McClory damages of £35,000 and McClory's court costs of £52,000, and future versions of the novel were credited as "based on a screen treatment by Kevin McClory, Jack Whittingham, and Ian Fleming" – in that order. Fleming conveyed to McClory the worldwide film rights to the novel Thunderball and McClory retained certain screen rights to the novel's story, plot, and characters. Harry Saltzman's and Albert R. Broccoli's production company Eon Productions later made a deal with McClory for Thunderball to be made into a film in 1965, with McClory producing. Under the deal, Eon licensed McClory's rights for a period of ten years and in return they assigned to McClory any rights they had in the scripts and treatments. McClory made an uncredited cameo in the film. By then, Bond was a box-office success, and series producers Broccoli and Saltzman feared a rival McClory film beyond their control; they agreed to McClory's producer's credit of a cinematic Thunderball, with them as executive producers.

In 1968 McClory announced plans to make a film about Irish revolutionary leader Michael Collins, to star Richard Harris. The film was to have been shot at Ardmore Studios in 1969 but was never made.

1970s–1980s
In 1975, McClory and Richard Harris took out a full-page ad in The Nassau Tribune "demanding an end to internment without trial" in Northern Ireland. Conservative opposition leader Edward Heath who was visiting Nassau at the time called a press conference and advised "Harris and McClory to 'ask their friends to stop murdering people.'"

In 1976, McClory announced he was to produce a second adaptation of Thunderball, to be titled either Warhead, Warhead 8, or James Bond of the Secret Service. The script ran into difficulties, after accusations from Danjaq and United Artists that the project had gone beyond copyright restrictions, which confined McClory to a film based only on the novel Thunderball; once again, the project was delayed. The project returned to the original nuclear terrorism plot of the original Thunderball, in order to avoid another lawsuit from Danjaq, and after McClory saw Jimmy Carter mention the issue in a 1980 presidential debate with Ronald Reagan. A final attempt by Fleming's trustees to block the film was made in the High Court in London in the spring of 1983, but this was thrown out by the court and the film, now titled Never Say Never Again, was permitted to proceed. Lord Justices Waller, Fox and May affirmed McClory's right to make James Bond films and enjoined the plaintiffs from taking similar legal action against McClory in the future. McClory went on to license his rights to Jack Schwartzman.

In 1988, he attempted an animated TV cartoon in partnership with a Dutch company, James Bond vs. S.P.E.C.T.R.E., but this never came to fruition, and James Bond Jr. was created as EON's counterattack to the aborted McClory animated attempt.

In 1989, McClory attempted to recycle the Warhead script again, retitling the project Atomic Warfare. He approached Pierce Brosnan who had missed out on the role of James Bond to Timothy Dalton due to his contract with NBC's Remington Steele. The film was supposed to be mainly set in Australia.

1990s–2000s
McClory subsequently continued attempts to make other adaptations of Thunderball, including Warhead 2000 A.D. which was to be made by Sony. MGM/UA took legal action against Sony and McClory in the United States to prevent the film going into production. MGM/UA abandoned the claim after settling with Sony. His rights were untouched. In 2004, Sony acquired 20% of MGM; however, the production and authority over everything involving the film version of James Bond is controlled by Eon Productions (Albert R. Broccoli's production company) and its parent company Danjaq, LLC. In 1992, McClory had to license the rights to producer Albert S. Ruddy for a proposed James Bond television program, but EON Productions blocked it, ending any hopes of a Bond TV show.

Prior to the settlement with MGM in 1999, Sony filed a lawsuit against MGM claiming McClory was the co-author of the cinematic 007 and was owed fees from Danjaq and MGM for all past films. This lawsuit was dismissed in 2000 on the ground that McClory had waited too long with his claims. The Ninth Circuit Court of Appeals later affirmed this decision in 2001.

2010s
On 15 November 2013, MGM and Danjaq LLC announced they had acquired all rights and interests of McClory's estate. MGM, Danjaq, and the McClory estate issued a statement saying that they had brought to an "amicable conclusion the legal and business disputes that have arisen periodically for over 50 years."

Personal life
McClory was married twice. He was survived by two sons and two daughters. His first wife was Frederica Ann "Bobo" Sigrist, daughter of Fred Sigrist. He later married Elizabeth O'Brien, daughter of the racehorse trainer Vincent O'Brien. They lived at Baltyboys House in Blessington, County Wicklow.

Death
McClory died on 20 November 2006, aged 82, at St. Columcille's Hospital in the Dublin suburb of Loughlinstown, from a cerebral hemorrhage, four days after the British release of Casino Royale.

license: Creative Commons - Attribution Share-Alike - https://creativecommons.org/licenses/by-sa/4.0/

title: Kevin McClory


text:
Variable camshaft timing

Variable camshaft timing (VCT) is an automobile variable valve timing technology developed by Ford. It allows for more optimum engine performance, reduced emissions, and increased fuel efficiency compared to engines with fixed camshafts. It uses electronically controlled hydraulic valves that direct high pressure engine oil into the camshaft phaser cavity. These oil control solenoids are bolted into the cylinder heads towards the front of the engine near the camshaft phasers. The powertrain control module (PCM) transmits a signal to the solenoids to move a valve spool that regulates the flow of oil to the phaser cavity. The phaser cavity changes the valve timing by rotating the camshaft slightly from its initial orientation, which results in the camshaft timing being advanced. The PCM adjusts the camshaft timing depending on factors such as engine load and RPM.

History
For twin-cam or DOHC engines, VCT was used on either the intake or exhaust camshaft. (Engines that have VCT on both camshafts are now designated as Ti-VCT.↓) The use of variable camshaft timing on the exhaust camshaft is for improved emissions, and vehicles with VCT on the exhaust camshaft do not require exhaust gas recirculation (EGR) as retarding the exhaust cam timing achieves the same result. VCT on the intake camshaft is used primarily for increasing engine power and torque as the PCM is able to optimize the opening of the intake valves to match the engine conditions.

VCT is used in Ford's Triton 5.4L 3-valve V8 engine, the Australian Barra 182 and 240 Inline-6s, and Ford's 4.6L 3-valve V8 engine used in the 2006-2010 Ford Explorer and 2005-2010 Ford Mustang GT.

The 2.0L Zetec inline-4 used in the 1998–2003 Ford Escort ZX2, Ford Contour, and 1999–2002 Mercury Cougar used VCT on the exhaust camshaft. The 2002–2004 SVT Focus (ST170 in Europe) also featured VCT, but on the intake camshaft of its modified version of the 2.0L Zetec engine. In addition, the 1.7L Zetec-S engine found in the European Ford Puma was equipped with variable camshaft timing. The 6.2L V8 introduced in the 2010 SVT Raptor also uses VCT. That motor has a single cam per bank, so it is dual-equal variable cam timing.

Ti-VCT
Twin independent variable camshaft timing (Ti-VCT) is the name given by Ford to engines with the ability to advance or retard the timing of both the intake and exhaust camshafts independently, unlike the original versions of VCT, which only operated on a single camshaft. This allows for improved power and torque, particularly at lower engine RPM, as well as improved fuel economy and reduced emissions. Some Ford Ti-VCT engines use BorgWarner's cam torque actuation (CTA) which utilizes the "existing torsional energy in the valve train to rotate the camshaft" instead of traditional oil pressure driven cam phasing.

Many new Ford engines feature Ti-VCT, including ones used in the 2011-2012 Mustangs, 2011 Edge and Edge Sport, 2011 Lincoln MKX, 2011 Fiesta, 2011 Explorer, 2011-2016 F-150, and 2012 Focus.

Engines using CTA system:

 * 5.0 Coyote

Engines without CTA:

 * 3.7 Cyclone

title: Variable camshaft timing


text:
User talk:Rsp

Hello and welcome to Wikipedia! Hope you like it here, and stick around.

Here are some tips to help you get started:

 * To sign your posts (on talk pages, for example) use the '~' symbol. To insert just your name, type ~~~ (3 tildes), or, to insert your name and timestamp, use ~~~~ (4 tildes).
 * Try the Tutorial, and feel free to experiment in the test area.
 * If you need help, post a question at the Help Desk
 * Follow the Simplified Ruleset
 * Eventually, you might want to read the Manual of Style and Policies and Guidelines.
 * Remember Neutral point of view
 * Explore, be bold in editing pages, and, most importantly, have fun!

Good luck!

Just a test

Rsp 17:15, 22 Jul 2004 (UTC)

title: User talk:Rsp


text:
1865 in art

Events from the year 1865 in art.

Events

 * July 21 – Charles Dodgson (Lewis Carroll) photographs Effie Gray Millais, John Everett Millais, and their daughters Effie and Mary at 7 Cromwell Place, London.
 * Ford Madox Brown completes his painting Work after thirteen years.
 * Morris, Marshall, Faulkner & Co. install the stained-glass east window in the chapel of St Edmund Hall, Oxford, England, designed by Edward Burne-Jones, William Morris and Philip Webb.
 * Édouard Manet's painting Olympia is first exhibited, at the Salon (Paris), and causes controversy.
 * Jean-François Millet's painting The Angelus (L'Angélus) is first exhibited and becomes very popular in France.
 * The Bargello in Florence becomes an art museum.

Works

 * Lawrence Alma-Tadema – An Egyptian at his Doorway
 * Albert Bierstadt
 * Looking Down Yosemite Valley, California
 * Staubbach Falls, near Lauterbrunnen, Switzerland
 * Ford Madox Brown – Work
 * Constantino Brumidi – The Apotheosis of Washington (fresco in United States Capitol rotunda)
 * Augustus Burke – Connemara Girl
 * Edward Burne-Jones and William Morris – The Crucifixion (stained-glass window for chapel of St Edmund Hall, Oxford)
 * Frederic Edwin Church – Aurora Borealis
 * Jean-Baptiste-Camille Corot – Ville d'Avray
 * Gustave Courbet
 * Portrait of Countess Karoly
 * Le ruisseau noir
 * Honoré Daumier – The Third-Class Carriage (National Gallery of Canada, Ottawa)
 * Edgar Degas – Medieval War Scene, his first painting exhibited at the Salon (Paris)
 * Thomas Faed – The Last of the Clan
 * William Powell Frith
 * Mary Elizabeth Maxwell (née Braddon)
 * The Marriage of the Prince of Wales
 * Jean-Léon Gérôme – Prayer
 * Henri Harpignies – Les Corbeaux
 * Henry Holiday – Stained glass windows for chapel of Worcester College, Oxford
 * Winslow Homer – The Veteran in a New Field
 * Elisabeth Jerichau-Baumann – A Wounded Danish Soldier
 * Sir Edwin Henry Landseer – Lady Godiva's Prayer (approximate date)
 * Andrew and George Anderson Lawson – Wellington's Column, Liverpool
 * Benjamin Williams Leader – Autumn's Last Gleam
 * Edward Lear – Jerusalem (Ashmolean Museum, Oxford)
 * Thomas Le Clear – Interior with Portraits
 * Édouard Manet
 * Angélina (Musée d'Orsay, Paris)
 * Bull-Fighting Scene (Private collection)
 * The Mocking of Christ (Art Institute of Chicago)
 * The Tragic Actor (Rouvière as Hamlet) (National Gallery of Art, Washington, D.C.)
 * George Hemming Mason – The Cast Shoe
 * Adolph Menzel – The Coronation of King William I in Königsberg 1861
 * John Everett Millais
 * Esther
 * Waking
 * Aimé Millet – Vercingétorix monument
 * Henry Moore – The Rainbow
 * Gustave Moreau – Thracian Girl Carrying the Head of Orpheus on His Lyre
 * Edward Poynter – Faithful unto Death
 * Val Prinsep – The Lady of the Tooti-Nameh or The legend of the parrot
 * Illarion Pryanishnikov – Jokers: Gostiny Dvor in Moscow
 * Dante Gabriel Rossetti – The Blue Bower
 * Alfred Sisley – Avenue of Chestnut Trees near La Celle-Saint-Cloud
 * John Tenniel – illustrations to Alice's Adventures in Wonderland Alice par John Tenniel 30.png illustration to Alice's Adventures in Wonderland]]
 * S. S. Teulon – Buxton Memorial Fountain (Westminster)
 * James McNeill Whistler – Rose and Silver: The Princess from the Land of Porcelain
 * Franz Xaver Winterhalter – Emperor Franz Joseph
 * Thomas Woolner – Godley Statue

Births

 * January 19 – Valentin Serov, Russian portrait painter (died 1911)
 * January 23 – Connie Gilchrist, English child actress and model (died 1946)
 * April 26 – Akseli Gallen-Kallela, Finnish painter (died 1931)
 * May 5 – Albert Aurier, French poet, art critic and painter, devoted to Symbolism (died 1892)
 * June 25 – Robert Henri, American painter, leader of the Ash Can School (died 1929)
 * June 26 – Bernard Berenson, Lithuanian-born American art historian (died 1959)
 * June 28 – David Young Cameron, Scottish painter (died 1945)
 * August 2 – John Radecki, Polish-born Australian stained glass artist (died 1955)
 * August 20 – Frank DuMond, American painter, illustrator and teacher (died 1951)
 * September 23 – Suzanne Valadon, French artists' model and painter (died 1938)
 * November 11 – Donatus Buongiorno, Italian-born American painter (died 1935)
 * December 28 – Félix Vallotton, Swiss painter and graphic artist (died 1925)
 * date unknown – Adelaïde Alsop Robineau, American painter and potter (died 1929)

Deaths

 * January 10 – William Fox-Strangways, 4th Earl of Ilchester, English diplomat and art collector (born 1795)
 * January 12 – Kunisada, Japanese designer of ukiyo-e woodblock prints (born 1786)
 * January 19 – Clementina Maude, Viscountess Hawarden, British portrait photographer (born 1822)
 * January 21 – Johan Erik Lindh, Swedish painter and former decorative painter who moved to Finland (born 1793)
 * January 23 – Joseph-Désiré Court, French painter of historical subjects and portraits (born 1797)
 * February 21 – Constant Troyon, French painter (born 1810)
 * April 21 – Josef Matěj Navrátil, Czech painter of murals and frescoes (born 1798)
 * April 28 – Robert William Sievier, English engraver, sculptor and inventor (born 1794)
 * June 18 – Antoine Wiertz, Belgian painter (born 1806)
 * July 11 – Ammi Phillips, American folk portrait painter (born 1788)
 * August 14 – Fitz Henry Lane, American Luminist marine painter (born 1804)
 * August 23 – Ferdinand Georg Waldmüller, Austrian painter and writer (born 1793)
 * September 17 – John Neagle, American portrait painter (born 1796)
 * September 23 – John Frederick Herring, Sr., English painter, signmaker and coachman in Victorian England (born 1795)
 * September 29 – François Joseph Heim, French painter (born 1787)
 * November 1 – Charles-François Lebœuf, French sculptor (born 1792)
 * December 24 – Charles Lock Eastlake, English painter and art collector (born 1793)
 * date unknown
 * Tivadar Alconiere, Hungarian painter (born 1797)
 * Michael Hanhart, English lithographer and chromolithographer (born 1788)

title: 1865 in art


text:
Frans Ackerman

Frans Ackerman (c. 1330–1387), Latinised as Franciscus Agricola, was one of the most famous Flemish statesmen and military leaders of the 14th century.

Life
Ackerman was born in Ghent. Rallying to Philip van Artevelde in the Ghent Revolt of 1379 against Louis II, Count of Flanders, Ackerman was placed in command of the Reisers, a mobile force of 3,000 men responsible for securing the city's supply-lines with Liège, Brussels and Leuven. He distinguished himself in the Battle of Beverhoutsveld (3 May 1382), which led to the taking of Bruges and put almost all of Flanders under the control of Ghent. At the head of some troops, he scoured the surrounding country for provisions and thus saved Ghent from being starved into submission.

With the king of France lending support to the count of Flanders, Ackerman undertook an embassy to England to seek the intervention of King Richard II. During his absence, the rebels suffered a serious defeat in the Battle of Roosebeke (27 November 1382), where Van Artevelde himself was slain. The count regained control of all of Flanders except the city of Ghent, where Ackerman became the rebel leader.

The English launched Despenser's Crusade in 1383, intervening in Flanders under the pretext of enforcing obedience to Pope Urban VI. Ackerman took Aardenburg from a French garrison, sacking the town and carrying the plunder to Ghent, and made an unsuccessful attempt on Bruges. Together with his English allies he was victorious at the Battle of Dunkirk (25 May 1383). He then took Oudenaarde by stratagem.

When the count died in 1384, he was succeeded by Philip the Bold, Duke of Burgundy, who had married the count's daughter, Margaret III, Countess of Flanders. Duke Philip continued the war. Ackerman took the town of Damme in a surprise attack, but was soon besieged within it by the army of Charles VI of France. The expected help from the English not arriving, his force broke out and returned to Ghent.

On 18 December 1385, the war ended with the Peace of Tournai between Ghent and Philip the Bold. Ackerman was a prominent member of the Ghent delegation who agreed the terms, but afterwards declined to serve the duke either at court or in the field.

On 22 July 1387, while on his way to Saint Peter's Abbey, Ghent, Ackerman was murdered by a son of the Lord of Herzele who blamed him for his father's death.

title: Frans Ackerman


text:
WNBA draft

The WNBA draft is an annual draft held by the WNBA through which WNBA teams can select new players from a talent pool of college and professional women's basketball players. The first WNBA draft was held in 1997.

Eligibility
The WNBA "requires players to be at least 22, to have completed their college eligibility, to have graduated from a four-year college or to be four years removed from high school". Since the WNBA draft is currently held in April, before most U.S. colleges and universities have ended their academic years, the league considers anyone scheduled to graduate in the 3 months after the draft to be a "graduate" for draft purposes. The current rules for draft eligibility have been in place since at least 2014.

The specifics of this rule differ in several ways from those used by the NBA for its draft.

 * Both drafts make a distinction between U.S. and "international" players. However, the definition of "international player" differs slightly between the two drafts. The NBA defines an "international player" as an individual who has permanently resided outside the U.S. for the three years preceding the draft while playing basketball (amateur or professional), did not complete high school education in the U.S., and has never enrolled in a U.S. college or university. A prospective NBA player's birthplace or citizenship is not relevant to his status as an "international player". On the other hand, the WNBA defines an "international player" as "any person born and residing outside the United States who participates in the game of basketball as an amateur or professional" (emphasis added), and who has never "exercised intercollegiate basketball eligibility" in the U.S. This means that a prospective WNBA player who was born in the United States is treated as a U.S. player, regardless of where she was educated or trained in basketball. Likewise, the association also defines as an "international player" a prospect with non-U.S. nationality even if one of her parents is a natural-born American, unless she has enrolled in a U.S. postsecondary institution.
 * The current age limit for NBA draft eligibility is 19, measured on December 31 of the calendar year of the draft. The WNBA's age limit is 20 for "international players" and 22 for U.S. players, both also being measured as of December 31 of the calendar year of the draft.
 * A WNBA prospect who graduates from college while under the age limit can be eligible, but only if the calendar year of her college graduation is no earlier than the fourth after her high school graduation.
 * In both drafts, players subject to the rules for U.S. players can declare early eligibility; however, the WNBA's higher age limit means that very few such players have the option to make such a declaration.
 * For those players who are eligible to declare early, the timing of the declaration process is dramatically different.
 * NBA prospects must notify the league office of their intent to enter the draft no later than 60 days prior to the draft, which is currently held in June. Current rules allow prospects to withdraw from the draft and retain college eligibility, as long as they comply with NCAA rules regarding relationships with agents, do not sign a professional contract, and notify the league office of their withdrawal no later than 10 days after the end of the NBA Draft Combine.
 * WNBA prospects must notify the league office no later than 10 days before the draft, and must renounce any remaining college eligibility to enter the draft. However, because postseason national tournaments (most notably the NCAA Division I tournament) are still ongoing during the 10 days prior to the draft, certain players who would otherwise be eligible to declare cannot do so before the standard deadline. A prospect whose team is still playing during the 10-day window must make her declaration within the 24 hours following her team's final game of the season, but no less than 3 hours before the scheduled start of the draft. The 3-hour period is a historic artifact that stems from the former scheduling of the WNBA draft; from 2006 to 2008, it was held in the city of the women's Final Four on the day after the championship game. Despite media commentary that argued that players involved in the NCAA tournament needed more time to make draft decisions, the most recent WNBA CBA, agreed to in 2020, did not change any draft eligibility rules.

For the 2021 draft only, the league and its players union, the Women's National Basketball Players Association, agreed to modified eligibility rules due to changes brought on by COVID-19. The most significant change is that all age-eligible college players who wished to enter that draft had to opt in. Because the NCAA ruled that the 2020–21 season would not count against the eligibility of any basketball player, everyone who played in that season, regardless of class, had remaining athletic eligibility at the time of the draft. Players who wished to enter the 2021 draft had to renounce college eligibility and notify the WNBA offices by email no later than April 1 of that year. Players involved in the 2021 Final Four had 48 hours after the completion of their final game, instead of the normal 24, to notify the league of their intent to enter the draft.

Structure
The 1997 WNBA draft was divided into three parts. The first part was the initial allocation of 16 players into individual teams. Players such as Cynthia Cooper and Michelle Timms were assigned to different teams. The second part was the WNBA Elite draft, which was composed of professional women's basketball players who had competed in other leagues. The last part would be the 4 rounds of the regular draft.

The next three seasons to follow 1998, 1999 and 2000 would all have expansion drafts. There would not be another expansion draft until the 2006 season.

All seasons before 2002 had 4 rounds. Since 2003, all drafts are 3 rounds.

In 2003 and 2004, there were dispersal drafts due to the folding of the Cleveland Rockers, Miami Sol and Portland Fire. The players from Rockers, Sol and Fire were reallocated to existing teams. There were also dispersal drafts in 2007 with the folding of the Charlotte Sting, 2009 with the shuttering of the Houston Comets, and in 2010 when the Maloofs cast off the Sacramento Monarchs to focus their resources on the Kings franchise in the NBA.

Players selected
There are no restrictions on what part of the world the players come from (though under varying rules, international players have been subject to tighter age restrictions within the draft than college players). However, college sports governing bodies, most notably the NCAA, prohibit players from competing in professional leagues simultaneously with their college eligibility. Once the player has joined the WNBA, she is eligible to participate in overseas leagues during the WNBA offseason (many WNBA players play in Europe, Australia, or more recently China).

First picks
Dena Head is the oldest No. 1 draft pick (she was 27 years old), having graduated from the University of Tennessee in 1992 and the first player ever drafted to the WNBA. Lauren Jackson is the youngest No. 1 draft pick, being drafted at the age of 19. As of 2012, six first picks have gone on to win WNBA Championships, with 12 rings among them. In the seventeen seasons that the WNBA has been in existence, eight No. 1 draft picks have helped lead their teams to a playoff berth in their rookie year.

 * Notes

title: WNBA draft


text:
Soyuz T-5

Soyuz T-5 was a human spaceflight into Earth orbit to the then new Salyut 7 space station in 1982. While the Soyuz-T was docked it received visits from the uncrewed Progress 13 resupply spacecraft, and the crewed Soyuz T-6 and Soyuz T-7.

The first crew hand launched an amateur radio satellite, the T-6 mission included a visiting Frenchman, and T-7 included the first woman in space in 20 years. It was the first mission to Salyut 7, but more than one spacecraft could be docked to S7 at a time, which is why the later missions could overlap with Soyuz T-5. The spacecraft launched with two people ("Elbrus crew"), and returned with three ("Dnieper crew").

Mission parameters

 * Mass: 6850 kg
 * Perigee: 190 km
 * Apogee: 231 km
 * Inclination: 51.6°
 * Period: 89.7 minutes

Mission highlights
This was the first (1st) expedition to the new Salyut 7 space station, launched into Earth orbit earlier in 1982. Salyut 7 was similar to the Salyut 6 (1977–1982) space station it superseded, but featured a number of improvements. The Soyuz T-5 spacecraft docked with Salyut 7 in orbit, and it was visited by the 2nd and 3rd expeditions to the space station. One advantage the new Salyut 7 station had over Salyut 6, was continuously available hot water.

The Elbrus crew ejected a 28-kg amateur radio satellite from a Salyut 7 trash airlock on May 17, 1982. The Soviets called this the first launch of a communications satellite from a crewed space vehicle. They did this ahead of the launch of two large geostationary satellites from the U.S. Space Shuttle (STS-5, November 11–16, 1982).

On May 25, the Elbrus crew reoriented Salyut 7 so the aft end of the Progress pointed toward Earth. This placed the station in gravity-gradient stabilization. Lebedev remarked in his diary that the attitude control jets were “very noisy,” and that they sounded like “hitting a barrel with a sledgehammer.” Of Salyut 7 during the unpacking of Progress 13, Lebedev said, “It looks like we’re getting ready to move or have just moved to a new apartment.” The following day the Elbrus crew closed the hatch from the work compartment into the intermediate compartment so the TsUP could pump fuel from Progress 13 to Salyut 7. The crew monitored the operation but played little active role in it. May 29 was spent organizing the supplies delivered. At the same time, according to Lebedev, “we filled the resupply ship with what we don’t need and tied them down with ropes. When I enter the resupply ship, it jingles with a metallic sound, so when we separate it will sound like a brass band.” Progress 13 pumped 300 liters of water aboard on May 31. On June 2 Progress 13 lowered the station's orbit to 300 km to receive Soyuz T-6.

In July, Valentin Lebedev, in charge of the plant experiments, reported that the Arabidopsis plants, chosen for their short 40-day lifecycle, had become the first plants to flower and produce seeds in the zero gravity of space, a Guinness World Record.

End of T-5
The Soyuz T-5 spacecraft was undocked in August 1982, leaving Salyut 7 and Soyuz T-7 spacecraft in orbit. The spacecraft returned to Earth successfully with Popov, Serebrov and Savitskaya, also called the "Dneiper crew". The Soyuz T-5 had been in space six weeks.

The initial "Elbrus crew", would return to Earth in the Soyuz T-7 spacecraft in December 1982.

title: Soyuz T-5


text:
1867 in art

Events from the year 1867 in art.

Events

 * Exposition Universelle in Paris helps popularize Japanese woodblock prints in the West.
 * Engravings of William Holman Hunt's The Finding of the Saviour in the Temple by Auguste III Blanchard are published by dealer Ernest Gambart in London in editions totalling 13,000.

Works

 * Frédéric Bazille – approximate date
 * Family Reunion
 * The Little Gardener
 * Portrait of Renoir
 * George Henry Boughton – Pilgrims Going To Church
 * William Burges – Narcissus washstand
 * Giuseppe Calì – Death of Dragut (Museum of Fine Arts, Valletta)
 * Julia Margaret Cameron – photographs
 * Carlyle Like a Rough Block of Michael Angelo's Sculpture
 * Profiles of Julie Jackson (her niece)
 * Frederic Edwin Church – Niagara Falls, from the American Side
 * Gustave Courbet – The kill of deer
 * Edgar Degas – The Bellelli Family completed (Musée d'Orsay, Paris)
 * Gustave Doré – engraved illustrations to Dante's Il Purgatorio ed il Paradiso
 * Jean-Léon Gérôme
 * Arnaut with two whippets
 * The Death of Caesar
 * Jerusalem, also known as Golgotha, Consumatum Est or The Crucifixion
 * Napoleon in Egypt
 * The runners of the Pasha
 * Western Wall
 * Artur Grottger
 * Phryne
 * Gustave Achille Guillaumet – The Sahara
 * Francesco Hayez
 * The Destruction of the Temple of Jerusalem
 * Odalisque
 * Frank Holl
 * Convalescent
 * Faces in the Fire
 * Ivan Kramskoi – Self-portrait
 * Sir Edwin Landseer
 * Bronze lions for Nelson's Column
 * The Wild Cattle of Chillingham
 * Charles-Auguste Lebourg – Games of Love (terracotta)
 * Frederic Leighton – Venus Disrobing for the Bath
 * Édouard Manet
 * L'Exposition universelle de 1867 ("The Universal Exhibition") (Nationalgalleriet, Oslo)
 * The Races at Longchamp
 * John Everett Millais – Sleeping
 * Claude Monet
 * Femme au jardin (Jeanne-Marguerite Lecadre in the Garden at Sainte-Adresse) (Hermitage Museum, Saint Petersburg)
 * Garden at Sainte-Adresse  (Metropolitan Museum of Art, New York)
 * Johannes Adam Simon Oertel – Rock of Ages
 * Vasily Perov – The Drowned
 * Edward Poynter – Israel in Egypt
 * Val Prinsep
 * Lisa (from Boccaccio's 'Decameron')
 * Miriam Watching the Infant Moses
 * Pierre-Auguste Renoir – Lise (with a Parasol)
 * Simeon Solomon – Carrying the Scrolls of the Law
 * Frederick Walker – Bathers
 * James McNeill Whistler – Symphony in White, No. 3

Births

 * January 17 – Louise Upton Brumback, American landscape painter (died 1929)
 * February 19 – Emília dos Santos Braga, Portuguese painter (died 1949)
 * March 8 – William de Leftwich Dodge, American muralist (died 1935)
 * March 10 – Leonard Raven-Hill, English illustrator (died 1942)
 * March 25 – Gutzon Borglum, American artist and sculptor (died 1941)
 * April 8 – Allen Butler Talcott, American painter (died 1908)
 * April 10 – George William Russell, Irish critic, poet and painter (died 1935)
 * May 12 - Frank Brangwyn, Welsh painter (died 1956)
 * June 8
 * Dagny Juel, Norwegian muse (murdered 1901)
 * O'Galop (Marius Rossillon), French cartoonist (died 1946)
 * July 5 – Max Jakob Friedländer, German-born curator and art historian (died 1958)
 * July 8 – Käthe Kollwitz, German graphic artist and sculptor (died 1945)
 * August 26 – Viktor Foerster, Czech painter and mosaic artist (died 1915)
 * September 9 – Ernst Oppler, German painter (died 1929)
 * September 14 – Charles Dana Gibson, American graphic artist (died 1944)
 * September 16 – Eva Watson-Schütze, American portrait photographer (died 1935)
 * September 19 – Arthur Rackham, English illustrator (died 1939)
 * October 3 – Pierre Bonnard, French painter (died 1947)
 * October 15 - Fujishima Takeji, Japanese painter (died 1943)
 * November 4 - Henry Charles Fehr, British sculptor (died 1940)
 * Undated
 * Florence Fuller, South African-born Australian painter (died 1946)
 * Pinckney Marcius-Simons, American painter (died 1909)

Deaths

 * January 4 – Marianne Ehrenström, Swedish writer, singer, painter, pianist, culture personality and memorialist (born 1773)
 * January 14 – Jean Auguste Dominique Ingres, French Neoclassical painter (born 1780)
 * February 10 – Carl Wagner, German Romantic landscape painter (born 1796)
 * February 28 – Jacques Raymond Brascassat, French painter (born 1804)
 * March – Kazimierz Jelski, Polish architect and sculptor (born 1782)
 * March 3 – J. L. Lund, Danish painter especially of historical subjects (born 1777)
 * March 6 – Peter von Cornelius, German painter (born 1784)
 * April 15 – Adelaide Ironside, Australian painter (born 1831)
 * May 18 – Clarkson Frederick Stanfield, English marine painter (born 1793)
 * September 15 – Alexis Joseph Depaulis, French sculptor and medallist (born 1792)
 * December 4 – Sophie Fremiet, French painter (born 1797)
 * December 22 – Théodore Rousseau, French landscape painter (born 1812)
 * December 27 – Antoine Claudet, French photographer and artist (born 1797)
 * December 29 – Carlo Marochetti, Italian-born sculptor (born 1805)
 * date unknown
 * Luo Bingzhang, Han Chinese official, military general, calligrapher and devout Confucian scholar (born 1793)
 * James Pollard, English painter and aquatint engraver especially of coach, fox hunting and equine scenes (born 1792)

title: 1867 in art