Kepler (spacecraft)

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This article is about Kepler space telescope. For the cargo spacecraft, see Johannes Kepler ATV.
Kepler
General information
NSSDC ID 2009-011A
Organization NASA
Major contractors Ball Aerospace & Technologies Corp.
Launch date 2009-03-07, 03:49:57.465 UTC[1]
Launched from Space Launch Complex 17-B
Cape Canaveral Air Force Station
Launch vehicle Delta II (7925-10L)
Mission length ≥ 3.5 years
elapsed: 2 years, 6 months and 8 days
Mass 1,039 kg (2,290 lb)
Type of orbit Earth-trailing heliocentric
Orbit height 1 AU
Orbit period 372.5 days
Wavelength 400–865 nm [2]
Diameter 0.95 m (3.1 ft)
Collecting area 0.708 m2 [3]
Website kepler.nasa.gov

Kepler is a NASA spacecraft equipped with a space observatory designed to discover Earth-like planets orbiting other stars.[4] The spacecraft is named in honor of German astronomer Johannes Kepler.[5] The spacecraft was launched on March 7, 2009,[6] with a planned mission lifetime of at least 3.5 years.[7]

The Kepler Mission is "specifically designed to survey a portion of our region of the Milky Way galaxy to discover dozens of Earth-size planets in or near the habitable zone and determine how many of the billions of stars in our galaxy have such planets."[8]

Keplers only instrument is a photometer that continuously monitors the brightness of over 145,000[9] main sequence stars in a fixed field of view. The data collected from these observations is analyzed to detect periodic fluctuations that indicate the presence of extrasolar planets (planets outside our solar system) that are in the process of crossing the face of other stars.

Kepler is a project under NASA's Discovery Program of relatively low-cost, focused science missions. The Ames Research Center is the home organization of the science principal investigator and is responsible for the ground system development, mission operations and science data analysis. Kepler mission development was managed by NASA's Jet Propulsion Laboratory until December 2009 but was then transferred to the Ames Research Center. Ball Aerospace & Technologies Corp. was responsible for developing the Kepler flight system.

The Kepler observatory is currently in active operation, with the first main results announced on 4 January 2010. As expected, the initial discoveries were all short-period planets, with longer period planets expected later. The first six weeks of data revealed five previously unknown planets, all very close to their stars.[10][11] Among the notable results are one of the least dense planets yet found,[12] and two low-mass white dwarf stars[13] that were initially reported as being members of a new class of stellar objects.[14]

On 2 February 2011, the Kepler team announced the results from the data of May to September 2009. They found 1235 planetary candidates circling 997 host stars, more than twice the number of currently known exoplanets. The Kepler results included 68 planetary candidates of Earth-like size and 54 planetary candidates in the habitable zone of their star. The team estimated that 5.4% of stars host Earth-size planet candidates and 17% of all stars have multiple planets. As the mission continues, additional longer period candidates continue to be found - as of September 2011, there were 1781 candidates.[15]

The next data release is scheduled for September 23, 2011, and will consist of one quarter (three months) of data through December 2009.[16] There will be no data released from 2010 or later until June 2012. Until these releases, the data collected after September 2009 is only available to Kepler team members. This slow release of data, much slower than the Kepler team promised[17] and opposed to the usual NASA policy of release within one year, has resulted in considerable criticism.[18][19][20][21] There is an exception to this data release policy; when the Kepler team itself publishes a paper on an object, the data used in the paper is released.[22]

Contents

[edit] Kepler spacecraft

Components of the Kepler telescope

The spacecraft has a mass of 1,039 kilograms (2,290 lb), has a 0.95-meter (37.4 in) aperture, and a 1.4-meter (55 in) primary mirror (when it was launched this was the largest on any telescope outside of Earth orbit).[23] The spacecraft 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 is a combined differential photometric precision (CDPP) of 20 ppm for a m(V)=12 solar-like star for a 6.5 hour integration, though the observations so far fall short of this objective (see mission status). An Earth-like transit produces a brightness change of 84 ppm and lasts for 13 hours when it crosses the center of the star.

[edit] Camera

Kepler image sensor array. The array is curved to account for Petzval field curvature.

The focal plane of the spacecraft's camera is made up of 42 CCDs at 2200 × 1024 pixels which makes it the largest camera launched into space with a resolution of 95 megapixels.[24][25] The array is cooled by heat pipes connected to an external radiator.[26] The CCDs are read out every six seconds (to limit saturation) and co-added on board for 30 minutes. However, even though at launch Kepler had the highest data rate of any NASA mission, the 30 minute sums of all 95 million pixels constitute more data than can be stored and sent back to Earth. Therefore the science team has pre-selected the relevant pixels associated with each star of interest, amounting to about 5 percent of the pixels. The data from these pixels is then requantized, compressed and stored, along with other auxiliary data, in the on-board 16 gigabyte solid-state recorder. Data that is stored and downlinked includes science stars, p-mode stars, smear, black level, background and full field-of-view images.[26]

The mission's life-cycle cost is estimated at US$600 million, including funding for 3.5 years of operation.[26]

[edit] Spacecraft history

Kepler's launch on March 7, 2009

In January 2006, the project was delayed eight months because of budget cuts and consolidation at NASA.[27] It was delayed again by four months in March 2006 due to fiscal problems.[27] 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.[27]

The observatory was launched on March 7, 2009 at 03:49:57 UTC (March 6, 10:49:57 p.m. EST) aboard a Delta II rocket from Cape Canaveral Air Force Station, Florida.[1][6] The launch was a complete 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.[28][29]

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.[30] 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.[31]

On May 12, 2009 at 5:01 p.m. Pacific Time (17:01 UTC-8), Kepler successfully completed its commissioning phase and began its search for planets around other stars.[32][33]

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.[34] On October 14, 2009, the cause of these safing events was determined to be a low voltage power supply which provides power to the RAD750 processor.[35] On January 12, 2010, one portion of the focal plane transmitted anomalous data, suggesting a problem with focal plane MOD-3 module, covering 2 out of Kepler's 42 CCDs. As of October 2010, the module was described as "failed", but the coverage still exceeded the science goals.[36]

Kepler downloads roughly 90-100 gigabits of science data[37] about once per month[38] - an example of such a download was on 22–23 November 2010.[39]

Once Kepler has detected a transit-like signature, it is necessary to rule out false positives with follow-up tests[40] such as doppler spectroscopy. Although Kepler was designed for photometry it turns out that it is capable of astrometry and such measurements can help confirm or rule out planet candidates.[41]

[edit] Performance

In terms of photometric performance, Kepler is working well, much better than any Earth-bound telescope, but still short of the 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 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.[42] Work to better understand, and perhaps calibrate out, instrument noise is ongoing.[43]

Since the signal from an Earth size planet is so close to the noise level (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. Recent estimates indicate a 7-8 year mission, as opposed to the 3.5 year planned, would be needed to find all transiting Earth-sized planets. The spacecraft has enough fuel for such a mission, but there is no funding for it so far.[44]

[edit] Spacecraft orbit and orientation

Kepler Mission search in context of Milky Way galaxy
The photometer's field of view in the constellations Cygnus, Lyra and Draco

The Kepler space observatory is in a Heliocentric orbit,[45][46] so that Earth does not occlude the stars, which are observed continuously, and so the photometer is not influenced by stray light from Earth. This orbit avoids the gravitational perturbations and torques inherent in an Earth orbit, allowing for a more stable viewing platform. The photometer points 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 the Sun. Cygnus is also a good choice to observe because it will never be obscured by Kuiper belt objects or the asteroid belt.[26]

An additional benefit of that choice is that Kepler is pointing in the direction of the Solar System's motion around the center of the galaxy. Thus, the stars which are observed by Kepler 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.

Kepler's orbit has been described by NASA as Earth-trailing.[47] With an orbital period of 372.5 days, Kepler slowly falls further behind Earth.

[edit] Spacecraft operations

Kepler's orbit. The solar array is adjusted at solstices and equinoxes

Kepler is operated out of Boulder, Colorado, USA, by the Laboratory for Atmospheric and Space Physics (LASP). The spacecraft's solar array will be rotated to face the Sun at the solstices and equinoxes. These rotations will be used to optimize the amount of sunlight falling on the solar array and to keep the heat radiator pointing towards deep space.[26] Together, LASP and Ball Aerospace & Technologies Corp. (who are responsible for building the spacecraft and instrument) control the spacecraft from the 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.

[edit] Communications

NASA contacts 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 4.33 Mbit/s. The Kepler spacecraft conducts its own partial analysis on board and only transmits scientific data deemed necessary to the mission in order to conserve bandwidth.[48]

[edit] Data management

Science data telemetry collected during mission operations at LASP is sent on for processing at the Kepler Data Management Center (DMC), located at the Space Telescope Science Institute on the campus of the 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 by the SO. During operations, the SOC (1) receives calibrated pixel data from the DMC, (2) applies the analysis algorithms to produce light curves for each star, (3) performs transit searches for detection of planets (threshold-crossing events, or TCEs) and (4) performs data validation of candidate planets by evaluating various data products for consistency as a way to eliminate false positive detections. The SOC also evaluates the photometric performance on an on-going 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).

[edit] Objectives and methods

The scientific objective of the Kepler mission is to explore the structure and diversity of planetary systems.[49] This is achieved by surveying a large sample of stars to achieve several goals:

Most of the extrasolar planets detected so far by other projects are giant planets, mostly the size of Jupiter and bigger. Kepler is 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.[51] For an Earth-like planet at 1 AU transiting a Sol-like star the probability is 0.465%, or about 1 in 215. At 0.72 AU (the orbital distance of Venus) the probability is slightly larger, at 0.65%; such planets could be Earth-like if the host star is a late G-type star such as Tau Ceti. In addition, because planets in a given system tend to orbit in similar planes, the possibility of multiple detections around a single star is actually rather high. For instance, if a Kepler-like mission conducted by aliens observed Earth transiting the Sun, there is a 12% chance that it would also see Venus transiting.

Kepler has a much higher probability of detecting Earth-like planets than the Hubble Space Telescope, since it has a much larger field of view (approximately 10 degrees square), and is dedicated to detecting planetary transits. The Hubble Space Telescope, in contrast, is used to address a wide range of 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[52] for observation, and they are observed simultaneously, with the spacecraft measuring variations in their brightness every 30 minutes. This provides a better chance for seeing a transit. In addition, the 1-in-215 probability means that if 100% of stars observed had the same diameter as the Sun, and each had one Earth-like terrestrial planet in an orbit identical to that of the Earth, Kepler would find about 465; but if only 10% of stars observed were such, then it would find about 46. The mission is well suited to determine the frequency of Earth-like planets orbiting other stars.[26][53]

Since Kepler must see at least three transits to be sure the dimming was caused by a planet, and since 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 will take longer, and discovering planets comparable to Earth is expected to take three years or longer.[45]

Data collected by Kepler is also being used for studying variable stars of various types and performing asteroseismology,[54] particularly on stars showing solar-like oscillations.[55]

[edit] Mission results to date

A photo taken by Kepler with two points of interest outlined. Celestial north is towards the lower left corner.
Detail of Kepler's image of the investigated area showing open star cluster NGC 6791. Celestial north is towards the lower left corner.
Detail of Kepler's image of the investigated area. The location of TrES-2b within this image is shown. Celestial north is towards the lower left corner.

[edit] 2009

NASA held a press conference to discuss early science results of the Kepler mission on August 6, 2009.[56] 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.[57][58]

Since Kepler's detection of planets depends on seeing very small changes in brightness, stars that vary in brightness all by themselves (variable stars) are not useful in this search.[38] From the first few months of data, Kepler scientists have determined that about 7,500 stars from the initial target list are such variable stars. These were dropped from the target list, and will be replaced by new candidates. On November 4, 2009, the Kepler project publicly released the light curves of the dropped stars.[59]

Ground-based follow-up studies of the first six weeks of data, revealed five previously unknown planets, all very close to their stars, one (Kepler-4b) slightly larger than Neptune and four (Kepler-5b, 6b, 7b and 8b) larger than Jupiter,[10] and Kepler-7b one of the least dense planets found yet.[12] Another discovery, not yet understood, was of at least two objects that are the size of planets, but hotter than their stars.[14] One analysis suggests these objects are white dwarfs.[60]

[edit] 2010

On 15 June 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 the Earth to larger than Jupiter. The identity and characteristics of 306 of the 706 targets were given. The released targets included 5 candidate multi-planet systems. Data for the remaining 400 targets with planetary candidates was to be released in February 2011. (For details about this later data release, see the Kepler results for 2011 below.) Nonetheless, the Kepler results, based on the candidates in the list released in 2010, imply that most candidate planets have radii less than half that of Jupiter. The Kepler results also imply that small candidate planets with periods less than 30 days are much more common than large candidate planets with periods less than 30 days and that the ground-based discoveries are sampling the large-size tail of the size distribution.[61] This contradicted older theories which had suggested small and Earth-like planets would be relatively infrequent.[62][63] Based on the Kepler data, an estimate of around 100 million habitable planets in our galaxy may be realistic.[64] However, some media reports of the TED talk have led to misunderstandings, apparently partly due to confusion concerning the term "Earth-like". By way of clarification, 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."[65][66][67]

[edit] 2011

Exoplanets in Kepler's FOV, in context of all discovered exoplanets (as of 2010-10-03), with some transit probabilities for example scenarios indicated

On 2 February 2011, the Kepler team announced the results of analysis of the data taken between 2 May and 16 September 2009.[68] They found 1235 planetary candidates circling 997 host stars. (The numbers that follow assume the candidates are really planets, though the official papers call them only candidates. Independent analysis indicates that at least 90% of them are real planets and not false positives.[69]) 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. 54 planets were within the habitable zone, including 5 less than twice the size of the Earth. 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. The observed planet count versus size increases to a peak at two to three times Earth-size and then declines inversely proportional to 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.[70]

[edit] Follow-ups by other teams

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.[71] Later, the same team then confirmed candidate KOI-423b.[72]

[edit] Citizen scientist participation

Kepler Mission data has recently[73] been used for the Zooniverse project "planethunters.org", which allows volunteers to look for transit events in the light curves to identify planets that the computer algorithms might miss. Currently, users may have found 69 candidates that were previously unrecognized by the Kepler Mission team.[74] The team has plans to publicly credit amateurs who spot such planets.

[edit] Extrasolar planets detected

Diagram of Kepler's investigated area with celestial coordinates (click for detail)
Kepler's first five exoplanets (click for detail)


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 extrasolar planet candidates is submitted to the Kepler Follow-up Program, or KFOP, to conduct follow-up observations.

Kepler has identified two systems containing objects which are smaller and hotter than their parent stars: KOI 74 and KOI 81.[75] These objects are probably low-mass white dwarf stars produced by previous episodes of mass transfer in their systems.[13]

In 2010, the Kepler team released a paper which had data for 312 extrasolar planet candidates from 306 separate stars. Only 33.5 days of data were available for most of the candidates.[61] NASA also announced data for another 400 candidates were being withheld to allow members of the Kepler team to perform follow-up observations.[76] The data for these candidates were made public on February 2, 2011.[68]

On February 2, 2011, the Kepler team released a list of 1235 extrasolar planet candidates, including 54 that may be in the "habitable zone."[77][78] 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).[79] 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).[80] Of all the new planet candidates, 68 are 125% of Earth's size or smaller, or smaller than all previously discovered exoplanets.[78] "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].[68] 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][68] are in the "habitable zone."[77] A more recent study found that one of these candidates (KOI 326.01) is in fact much larger and hotter than first reported.[81]

Based on the latest Kepler findings, astronomer Seth Shostak estimates that "within a thousand light-years of Earth," there are "at least 30,000" habitable planets.[82] 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.[83] In March 2011, astronomers at NASA's Jet Propulsion Laboratory (JPL) reported that about "1.4 to 2.7 percent" of all sunlike stars are expected to have earthlike planets "within the habitable zones of their stars". This means there are "two billion" of these "Earth analogs" in our own Milky Way galaxy 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.[84]

[edit] Confirmed planets

Below is a table of all extrasolar planetary systems found by Kepler (from the list of extrasolar planets). The first three of the list were already known prior to Kepler, all the others are new discoveries. As of September 15, 2011, 683 known extrasolar planets (in 561 planetary systems and 80 multiple planet systems) are listed in the Extrasolar Planets Encyclopaedia, ranging from the size of terrestrial planets somewhat larger than Earth to gas giants larger than Jupiter.[85]

Star Kepler Input
Catalog
(KIC)		 Constell.
 Right
ascension		 Declination
 App.
mag.		 Distance
(ly)		 Spectral
type		 Planet Mass
(MJ)		 Radius
(RJ)		 Orbital
period
(d)		 Semimajor
axis
(AU)		 Orbital
ecc.		 Inclin.
(°)		 Discovery
year
TrES-2 KIC 11446443 Draco 19h 07m 14s +49° 18′ 59″ 11.41 750 G0V TrES-2b
(Kepler-1b)		 1.199 1.272 1.49 0.036 0 83.62 2006
HAT-P-7 KIC 10666592 Cygnus 19h 28m 59s +47° 58′ 10″ 10.46 1044 F8 HAT-P-7b
(Kepler-2b)		 1.776 1.363 2.20 0.038 0 85.7 2008
HAT-P-11 KIC 10748390 Cygnus 19h 50m 50.2s +48° 04′ 51.1″ 9.59 123 K4 HAT-P-11b
(Kepler-3b)		 0.081 0.422 4.89 0.053 0.198 88.5 2009
Kepler-4 KIC 11853905 Draco 19h 2m 27.7s +50° 8′ 8.7″ 12.6 1794 Kepler-4b 0.077 0.357 3.21 0.046 0 89.76 2010
Kepler-5 KIC 8191672 Cygnus 19h 57m 37.7s +44° 2′ 6.2″ 13.9 Kepler-5b 2.114 1.431 3.55 0.051 0 86.3 2010
Kepler-6 KIC 10874614 Cygnus 19h 47m 20.9s +48° 14′ 23.8″ 13.8 Kepler-6b 0.669 1.323 3.23 0.046 0 86.8 2010
Kepler-7 KIC 5780885 Lyra 19h 14m 19.6s +41° 5′ 23.3″ 13.3 Kepler-7b 0.433 1.478 4.89 0.062 0 86.5 2010
Kepler-8 KIC 6922244 Lyra 18h 45m 9.1s +42° 27′ 3.8″ 13.9 4338 Kepler-8b 0.603 1.419 3.52 0.048 0 84.07 2010
Kepler-9 KIC 3323887 Lyra 19h 2m 17.76s +38° 24′ 3.2″ 13.9[86] 2300 G2V Kepler-9b 0.252 0.842 19.24 0.14 0.15 88.55 2010
Kepler-9 KIC 3323887 Lyra 19h 2m 17.76s +38° 24′ 3.2″ 13.9[86] 2300 G2V Kepler-9c 0.171 0.823 38.91 0.225 0.13 88.12 2010
Kepler-9 KIC 3323887 Lyra 19h 2m 17.76s +38° 24′ 3.2″ 13.9[86] 2300 G2V Kepler-9d 0.022? 0.15 1.59 0.027  ?  ? 2010
Kepler-10 KIC 11904151 Draco 19h 2m 43s +50° 14′ 29″ 10.96 564 G Kepler-10b 0.0143 0.127 0.837 0.017 0 84.4 2011
Kepler-10 KIC 11904151 Draco 19h 2m 43s +50° 14′ 29″ 10.96 564 G Kepler-10c < 0.063 0.199 45.29 0.241 0 89.65 2011
Kepler-11 KIC 6541920 Cygnus 19h 14m 27.62s +41° 54′ 32.9″ 14.2 1999 GV Kepler-11b 0.01353 0.1762 10.30 0.091 0 88.5 2011[87]
Kepler-11 KIC 6541920 Cygnus 19h 14m 27.62s +41° 54′ 32.9″ 14.2 1999 GV Kepler-11c 0.0425 0.28175 13.03 0.106 0 89 2011[87]
Kepler-11 KIC 6541920 Cygnus 19h 14m 27.62s +41° 54′ 32.9″ 14.2 1999 GV Kepler-11d 0.01919 0.3068 22.69 0.159 0 89.3 2011[87]
Kepler-11 KIC 6541920 Cygnus 19h 14m 27.62s +41° 54′ 32.9″ 14.2 1999 GV Kepler-11e 0.02643 0.4043 32.00 0.194 0 88.8 2011[87]
Kepler-11 KIC 6541920 Cygnus 19h 14m 27.62s +41° 54′ 32.9″ 14.2 1999 GV Kepler-11f 0.007237 0.2335 46.69 0.25 0 89.4 2011[87]
Kepler-11 KIC 6541920 Cygnus 19h 14m 27.62s +41° 54′ 32.9″ 14.2 1999 GV Kepler-11g < 0.95 0.3274 118.38 0.462 0 89.8 2011[87]
Kepler-14 KIC 10264660 Lyra 19h 10m 50s +47° 19′ 59″ 12.12 3196 F Kepler-14b 8.4 1.136 6.790123 - 0.035 90 2011[88]

The planets KOI-423b[72] and KOI-428b.[71] KOI=Kepler Object of Interest.

[edit] Kepler Input Catalog

Main article: Kepler Input Catalog

The Kepler Input Catalog (or KIC) is a publicly searchable database of roughly 13.2 million targets used for the Kepler Spectral Classification Program and Kepler.[89][90] The catalog alone is not used for finding Kepler targets, because only a portion (about 1/3 of the catalog) can be observed by the spacecraft.[89]

[edit] See also

[edit] References

  1. ^ a b Aarhus University Staff (14 March 2009). "KASC Scientific Webpage". Kepler Asteroseismic Science Consortium. http://astro.phys.au.dk/KASC/. Retrieved 2009-03-14. 
  2. ^ NASA Staff (2010). "Kepler Mission: Photometer and Spacecraft". NASA. http://kepler.nasa.gov/Mission/QuickGuide/MissionDesign/PhotometerAndSpacecraft/. Retrieved 2011-02-02. 
  3. ^ Aperture of 0.95 m yields a light-gathering area of Pi×(0.95/2)2 = 0.708 m2; the 42 CCDs each sized 0.050 m × 0.025m yields a total sensor area of 0.0525 m2: [1]
  4. ^ Koch, David; Gould, Alan (March 2009). "Kepler Mission". NASA. http://www.kepler.arc.nasa.gov/. Retrieved 2009-03-14. 
  5. ^ DeVore, Edna (9 June 2008). "Closing in on Extrasolar Earths". SPACE.com. http://www.space.com/searchforlife/080619-seti-extrasolar-earths.html. Retrieved 2009-03-14. 
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