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Kepler-186[1]

Kepler-186 is indicated by the red circle (2MASS J band image)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cygnus[2]
Right ascension 19h 54m 36.6535s[3]
Declination +43° 57′ 18.026″[3]
Apparent magnitude (V) 15.29[4]
Characteristics
Evolutionary stage Main sequence[3]
Spectral type M1V[5]
Astrometry
Proper motion (μ) RA: 2.171(18) mas/yr[3]
Dec.: −4.363(20) mas/yr[3]
Parallax (π)5.6336±0.0169 mas[3]
Distance579 ± 2 ly
(177.5 ± 0.5 pc)
Details
Mass0.544 ± 0.02[5] M☉
Radius0.523 ± 0.02[5] R☉
Luminosity (bolometric)0.055 +0.011
−0.006[5] L☉
Temperature3755 ± 90[5] K
Metallicity [Fe/H]−0.26 ± 0.12[5] dex
Rotation34.404±0.075 days[6]
Age4.0 ± 0.6[5] Gyr
Other designations
KIC 8120608[7], KOI-571,
2MASS J19543665+4357180, Gaia DR2 2079000330051813504
Database references
SIMBADdata

Kepler-186 is a main-sequence M1-type dwarf star, located 177.5 parsecs (579 light years) away in the constellation of Cygnus. The star is slightly cooler than the sun, with roughly half its metallicity. It is known to have five planets, including the first Earth-sized world discovered in the habitable zone: Kepler-186f.[8] The star hosts four other planets discovered so far, though they all orbit interior to the habitable zone.

Within two first years of gathered data, the signals of four inner planetary candidates were found. Discussion of planets in the system was taking place in August and November 2013.[9] In February 2014, those planets were confirmed through the "verification by multiplicity" method. The fifth outermost candidate was confirmed in the same manner in April 2014.[10] The possibility that the signals in the light curve of the star were actually from something else has been ruled out by an investigation with the W. M. Keck and Gemini Observatories, using speckle imaging and adaptive optics techniques, which, while unable to resolve the planets, were able to rule out other possibilities than the system of planets.[11]

Naming

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The Kepler Space Telescope search volume, in the context of the Milky Way Galaxy.

Kepler project

[edit]

As the Kepler space telescope observational campaign progressed initial identifications of systems were entered in the Kepler Input Catalog (KIC), and then progressed as a candidate host of planets as Kepler Object of Interest (KOI). Thus Kepler-186 started as KIC 8120608 and then was identified as KOI 571.[12] Planetary candidates were detected around the star by NASA's Kepler Mission, a mission tasked with discovering planets in transit around their stars. The transit method that Kepler uses involves detecting dips in brightness in stars. These dips in brightness can be interpreted as planets whose orbits pass in front of their stars from the perspective of Earth, although other phenomena can also be responsible which is why the term planetary candidate is used.[13]

Outside the Kepler project

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Outside of the Kepler project, the 2MASS survey catalogued this star as 2MASS J19543665+4357180.[1]

Star

[edit]

A number of previously unknown measurements of the star are known.[14][15] In the infrared/microwave EM spectrum[1] its H band magnitude is 11.605, J band magnitude is 12.473, and its K band magnitude is 11.605. In the visual Photometric system magnitude it is 14.90(R)(towards the red end of the visual spectrum) and 16.40(B)(the blue end of the spectrum)[14] (see also Apparent magnitude.) It is a BY Draconis variable changing brightness slightly, probably from star-spots, with a period of 33.695 days.[16]

The star is an M-type red dwarf, bordering on being a K-type orange dwarf, with a mass 0.544 times that of the Sun's and a density of 5.29 g/cm3.[5]

Planetary system

[edit]
The Kepler-186 planetary system[8]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ~1.24 M🜨 0.0343±0.0046 3.8867907 <0.24 83.56° 1.07±0.12 R🜨
c ~2.1 M🜨 0.0451±0.0070 7.267302 <0.24 85.94° 1.25±0.14 R🜨
d ~2.54 M🜨 0.0781±0.0010 13.342996 <0.25 87.09° 1.4±0.16 R🜨
e ~2.15 M🜨 0.11±0.015 22.407704 <0.24 88.24° 1.27±0.15 R🜨
f 1.44+2.33
−1.12 M🜨 		0.432±0.01 129.9444 <0.04 89.9° 1.17±0.08 R🜨
Size comparison of Kepler-186f (artist's impression) with Earth along with their projected habitable zones

The five planets discovered around Kepler-186 are all expected to have a solid surface. The smallest one, Kepler-186b, is only 8% larger than Earth, while the largest one, Kepler-186d, is almost 40% larger.

The four innermost planets are probably tidally locked, but Kepler-186f is farther out, where the star's tidal effects are much weaker, so there may not have been enough time for its spin to slow down that much. Because of the very slow evolution of red dwarf stars, the age of the Kepler-186 system is poorly constrained, although it is likely to be greater than a few billion years.[17] There is a roughly 50-50 chance it is tidally locked. Since it is closer to its star than Earth is to the Sun, it will probably rotate much more slowly than Earth; its day could be weeks or months long (see Tidal effects on rotation rate, axial tilt and orbit).[18]

Planetary formation simulations have also shown that there could be one additional non-transiting low-mass planet between Kepler-186e and Kepler-186f. If this planet exists, it is likely not much more massive than Earth. If it were, its gravitational influence would likely prevent Kepler-186f from transiting.[17] Conjectures involving the Titius–Bode law, (and the related Dermott's law) indicate that there could be several remaining planets to be found in the system - two small ones between e and f and another larger one outside of f.[19] That hypothetical outer planet must have an orbital radius beyond 16.4 AU for planetary system to remain stable.[20]

The low metallicity of the star at a metallicity (dex) of -0.26, or to put it another way, about half that of the Sun's,[8] is associated with a decreased chance of planets overall and giant planets specifically but an increased chance of Earth sized planets, in a general study of stars.[21]


See also

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References

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[edit]
Revisions and contributorsEdit on WikipediaRead on Wikipedia

Kepler-186

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Kepler-186 is an M-type red dwarf star located approximately 580 light-years away in the constellation Cygnus, orbited by five super-Earth-sized exoplanets, including the Earth-sized candidate Kepler-186f, which was the first such planet reported in the habitable zone of another star.[1] However, recent analyses as of 2025 have raised doubts about the detection reliability of Kepler-186f, with a false alarm probability of around 20%.[2] The star has a mass of about 0.48 times that of the Sun, a radius of 0.46 solar radii, and an effective temperature of 3881 K, making it a cool, dim host compared to our Sun.[1] The Kepler-186 system was discovered in 2014 using the transit method by NASA's Kepler Space Telescope, which detected periodic dips in the star's brightness caused by the planets passing in front of it.[1] The planets, designated b through f in order of increasing orbital distance, all have radii between 1.07 and 1.40 times that of Earth, with orbital periods ranging from 3.9 days for the innermost (Kepler-186b) to 130 days for the outermost (Kepler-186f).[1] Masses for the planets are not precisely determined, though estimates suggest they are rocky super-Earths similar in composition to Earth.[1] Kepler-186e and Kepler-186f orbit within the star's habitable zone, the region where conditions might allow for liquid water on a planet's surface, with Kepler-186f receiving about one-third of the solar flux Earth does from the Sun.[1] This discovery marked a milestone in exoplanet research, demonstrating that Earth-sized worlds can exist in potentially habitable environments around cool red dwarfs, which comprise about 75% of stars in the Milky Way.[3] Despite its promise, Kepler-186f's actual habitability remains uncertain due to factors like tidal locking and potential stellar flares from the active red dwarf host, in addition to questions about its very detection.[3]

Discovery

Transit detection

The Kepler Space Telescope, launched in March 2009, conducted its primary mission through May 2013, during which it continuously monitored the photometric variability of approximately 150,000 stars within a 115-square-degree field of view centered on the constellations Cygnus and Lyra.[4] This survey employed high-precision photometry to detect periodic diminutions in stellar brightness, characteristic of planetary transits, using a photometer with a 95-centimeter aperture that sampled light curves every 30 minutes in long cadence mode.[4] The Kepler-186 system was detected through the identification of multiple periodic transit signals in the host star's light curve, spanning data from Quarters 1 to 17 (covering March 2009 to May 2013).[1] The Transiting Planet Search (TPS) module of the Kepler pipeline processed these pre-searched time series after systematic corrections, applying a wavelet-based detection algorithm to identify threshold-crossing events indicative of transiting bodies, including both single-planet and multi-planet configurations.[5] Initial planet candidates for the inner four planets (Kepler-186b through e) were flagged as Kepler Objects of Interest (KOI-571.01 to .04) in catalogs released between 2011 and 2013, based on data from Quarters 1-6 through Q1-12, while the outermost planet (Kepler-186f, KOI-571.05) required the extended baseline for detection due to its longer orbital period.[3] Transit depths for the system ranged from 46.7 ppm (0.0047%) for Kepler-186f to 514 ppm (0.051%) for Kepler-186b, reflecting the relative sizes of the planets compared to the small M-type host star.[1] These signals achieved signal-to-noise ratios of approximately 36 to 50, enabling robust detection above the pipeline's multiple-event threshold while distinguishing them from stellar variability or instrumental noise.[1] False positive elimination involved detailed pixel-level analysis of the full-frame images, including flux-weighted centroid calculations during transit events to measure any offset from the target star's position; for Kepler-186, centroids showed no significant displacement (less than 0.1 pixels), confirming the signals originated on-target rather than from background eclipsing binaries or contaminating sources. Additional diagnostics, such as difference images and phase-folded light curve fits, further supported the planetary nature of the detections with no evidence of astrophysical false positives.[6]

Confirmation process

Following the initial detection of transit signals by the Kepler space telescope, the confirmation of the Kepler-186 system relied on the "verification by multiplicity" statistical method, which assesses the low likelihood of false positives in multi-planet configurations. This technique, applied to the four inner planet candidates (b through e), calculated a false positive probability of less than 1% for the system, given the improbability of multiple independent false positive events aligning in the same star field.[7] To further validate the candidates and exclude alternatives like eclipsing binaries, ground-based high-resolution imaging observations were performed using the NIRC2 instrument on the Keck II telescope and the NIRI instrument on the Gemini North telescope during 2013 and 2014. These observations detected no nearby companions brighter than the difference in magnitude limits (Δm ≈ 5.5 at 1″ separation for Keck and Δm ≈ 4.5 at 1″ for Gemini), providing strong evidence against blended eclipsing binary scenarios and supporting the planetary interpretation with over 99% confidence.[3] The four inner planets were officially validated and announced on February 27, 2014, through a comprehensive analysis published by Rowe et al., marking one of the first applications of multiplicity verification to confirm dozens of Kepler systems simultaneously. Kepler-186f, the outermost planet, was subsequently identified in extended Kepler data and confirmed using refined transit modeling integrated with the system's multiplicity, achieving a false positive probability below 0.02%; it was announced on April 17, 2014, via a NASA press release accompanying the seminal paper by Quintana et al. in Science.[7][8][3]

Nomenclature

Star designation

The host star of the Kepler-186 planetary system is designated Kepler-186 in accordance with the naming conventions adopted by NASA's Kepler mission for stars hosting confirmed exoplanets, a practice formalized following the mission's extension in 2012 to prioritize validated discoveries.[9] This identifier was assigned upon the confirmation of its five transiting planets in 2014.[3] The designation traces its origins to the Kepler Input Catalog (KIC) entry KIC 8120608, which cataloged potential target stars for observation, and the subsequent Kepler Object of Interest (KOI) number KOI-571, assigned to the system after initial transit signals were detected during the mission's primary survey phase from 2009 to 2013.[1] These catalogs facilitated the systematic identification and follow-up of exoplanet candidates around faint stars in the Kepler field.[10] Additional catalog references for the star include the Two Micron All Sky Survey identifier 2MASS J19543665+4357180, based on its infrared photometry, and the Gaia Data Release 3 source identifier 2079000330051813504, which incorporates astrometric data from the European Space Agency's Gaia mission.[1] The Gaia DR3 parallax measurement of 5.6336 ± 0.0169 mas from 2022 refines the system's distance to 579 ± 2 light-years (177.5 ± 0.5 parsecs).[11] No proper name has been officially assigned to the star by the International Astronomical Union (IAU), consistent with IAU guidelines that reserve proper names for select exoplanet host stars through public naming campaigns rather than systematic application to all discoveries.

Planet designations

The planets orbiting the star Kepler-186 are systematically designated as Kepler-186b, Kepler-186c, Kepler-186d, Kepler-186e, and Kepler-186f, following the standard exoplanet nomenclature established by the International Astronomical Union (IAU). This format appends a lowercase letter to the host star's catalog name to identify each planet individually.[1] The lettering begins with 'b' for the innermost planet and proceeds sequentially to 'f' for the outermost, ordered by increasing semi-major axis rather than discovery sequence, as per IAU guidelines for multi-planet systems. This assignment ensures a consistent, distance-based hierarchy that distinguishes the planets' positions within the system architecture.[3] Prior to confirmation, the planetary candidates were cataloged as Kepler Objects of Interest (KOIs) under the designation KOI-571, with specific identifiers KOI-571.01 (Kepler-186c), KOI-571.02 (Kepler-186d), KOI-571.03 (Kepler-186b), KOI-571.04 (Kepler-186e), and KOI-571.05 (Kepler-186f), reflecting their initial detection in Kepler mission data without final orbital ordering.[12] These provisional KOI labels, managed by NASA's Kepler project, served as temporary markers for transit-like signals during the vetting process, distinct from the permanent IAU-approved names assigned post-validation.[7] The Kepler-186 planets lack any IAU-approved proper names and are exclusively referenced by these systematic designations in major exoplanet catalogs, such as the NASA Exoplanet Archive.[1] This adherence to the host star's Kepler-186 identifier maintains uniformity across astronomical databases.

Host star

Physical characteristics

Kepler-186 is a red dwarf star of spectral type M1V, characteristic of cool, low-mass main-sequence stars. Its effective temperature is measured at 3876 ± 157 K, significantly cooler than the Sun's 5772 K, contributing to its reddish appearance and lower energy output.[1] The star's mass is 0.543 ± 0.020 M⊙, about half that of the Sun, with a radius of 0.548 ± 0.016 R⊙. These dimensions result in a luminosity of 0.061 L⊙, derived from Gaia DR3 astrometry combined with spectral energy distribution (SED) fitting to multi-wavelength photometry. The metallicity, an indicator of heavy element abundance relative to hydrogen, is [Fe/H] = -0.31 +0.11/-0.09 dex, suggesting a slightly metal-poor composition compared to the Sun. Kepler-186 lies at a distance of 579 ± 2 light-years in the constellation Cygnus.[1][13] More recent estimates from the TESS Input Catalog version 8 (TICv8; Stassun & Gaudi 2019), incorporating Gaia DR3 data as of 2023, refine these parameters for improved precision in exoplanet system modeling.[1] The star's luminosity is approximated by the Stefan-Boltzmann relation for blackbody radiation:
LL⊙=(RR⊙)2(TT⊙)4 \frac{L}{L_\odot} = \left( \frac{R}{R_\odot} \right)^2 \left( \frac{T}{T_\odot} \right)^4
Substituting the measured radius (0.548 R⊙) and effective temperature (3876 K, with T⊙ = 5772 K) yields approximately 0.061 L⊙, consistent with the SED-derived luminosity and highlighting the star's subdued radiative output. This low luminosity influences the insolation levels received by orbiting bodies.[1]

Activity and age

The rotation period of Kepler-186, an early M dwarf, is measured at approximately 34 days based on photometric variability in Kepler light curves, indicating rotational modulation from starspots.[13] This period aligns with expectations for mid-M dwarfs, which exhibit relatively slow rotation compared to more active younger stars. The photometric activity index, derived from the amplitude of these variations, is low at around 3270 ppm, consistent with subdued magnetic activity typical of such stars in this evolutionary stage.[14] The estimated age of Kepler-186 is 4.0 ± 0.6 billion years, obtained through gyrochronology relations calibrated to the rotation period and supplemented by isochrone fitting to stellar evolutionary models.[13] This places the star in a mature phase, where magnetic activity has declined from its youth, reducing the potential for high-energy events that could influence nearby planetary environments. Flare activity on Kepler-186 is rare, with no significant events detected in the full Kepler dataset; any undetected flares contribute less than 0.1% of the star's total optical energy output.[14] Such low flare rates suggest minimal erosive impact on planetary atmospheres from stellar coronal mass ejections or high-energy radiation, though the implications for habitability depend on planetary magnetic protection and atmospheric composition.[15] As of observations through 2025, no significant radial velocity jitter has been reported for Kepler-186, attributable to its faintness (V ≈ 14.6 mag) limiting high-precision spectroscopic follow-up; existing measurements show only the systemic velocity without notable variability.[13]

Planetary system

System architecture

The Kepler-186 planetary system is a compact multi-planet configuration featuring five transiting planets in near-circular orbits around an M1-type dwarf star, with semi-major axes spanning from approximately 0.038 AU for the innermost planet to 0.393 AU for the outermost.[1] This architecture places all planets within a relatively close radial range, characteristic of many multi-planet systems detected by the Kepler mission, and reflects the dynamical packing typical of systems around cool, low-mass stars.[16] The orbital periods of the planets increase monotonically outward, ranging from 3.89 days for Kepler-186b to 129.95 days for Kepler-186f, resulting in a period ratio distribution that shows no confirmed mean-motion resonances but includes near 4:1 ratios among the outer planets.[16][1] Orbital eccentricities are low across the system, consistent with circular orbits (e < 0.1), which contributes to the overall dynamical quietness. Long-term N-body simulations, assuming planetary masses below 10 Earth masses, demonstrate that the system remains stable for timescales exceeding 1 Gyr, with no significant perturbations leading to ejections or collisions.[16] The detection of the outermost planet, Kepler-186f, is controversial, with a false alarm probability of approximately 20% based on recent reassessments.[2][17] Insolation levels in the system vary sharply with orbital distance, driven by the host star's luminosity of approximately 0.061 times that of the Sun, which scales the incident stellar flux relative to Earth.[1] The inner planets receive approximately 2.6 to 26 times Earth's insolation, creating hot environments, while the outermost planet receives about 0.25 times Earth's level, positioning it near the inner edge of the system's habitable zone.[1]

Planet properties

The planets in the Kepler-186 system are classified as super-Earths, with their radii derived from the depths of their transits relative to the host star's radius. Kepler-186b has a radius of 1.05 ± 0.13 R⊕, Kepler-186c 1.23 ± 0.16 R⊕, Kepler-186d 1.53 ± 0.20 R⊕, Kepler-186e 1.26 ± 0.17 R⊕, and Kepler-186f 1.06 ± 0.14 R⊕.[1] Masses for these planets remain uncertain in the absence of radial velocity detections, relying instead on mass-radius models calibrated from known exoplanets. Kepler-186f is estimated at 1.71 ± 0.45 M⊕, while the inner planets (b through e) fall in the approximate range of 1–3 M⊕ depending on assumed bulk compositions.[18] Based on their radii and modeled densities, the inner four planets (b, c, d, and e) are likely composed primarily of rock or substantial water/ice layers, consistent with terrestrial or ocean-world structures. Kepler-186f is potentially rocky as well, though some models permit a thin hydrogen/helium envelope that could influence its atmosphere.[16] Equilibrium temperatures, calculated assuming zero albedo and no heat redistribution, range from approximately 320–580 K for the inner planets due to their proximity to the host star, while Kepler-186f has a cooler value of ~180 K.[1]
PlanetRadius (R⊕)Estimated Mass (M⊕)Equilibrium Temperature (K)
Kepler-186b1.05 ± 0.13~1–3578
Kepler-186c1.23 ± 0.16~1–3469
Kepler-186d1.53 ± 0.20~1–3383
Kepler-186e1.26 ± 0.17~1–3322
Kepler-186f1.06 ± 0.141.71 ± 0.45179

Habitability

Kepler-186f assessment

Kepler-186f occupies a position within the conservative habitable zone of its M1V host star, which extends from approximately 0.22 to 0.40 AU based on updated climate models accounting for moist and maximum CO2 greenhouse limits.[19] At an orbital semi-major axis of 0.40 AU, the planet receives an insolation flux of 0.32^{+0.06}_{-0.04} times that of Earth, placing it near the outer edge of this zone where stellar radiation is sufficient to potentially sustain liquid surface water under favorable atmospheric conditions.[20] The planet's orbital configuration may result in tidal locking to its host star, given the slow pace of tidal evolution influenced by its initial spin and the system's age.[16] If locked, this would create persistent day and night sides, concentrating habitability prospects in the terminator region where moderate temperatures could prevail; alternatively, non-synchronous rotation might allow more uniform climate distribution. Surface composition models indicate Kepler-186f could feature either a global ocean or exposed rocky terrain, both compatible with its estimated Earth-like density and radius of 1.11 R⊕.[16] Climate simulations incorporating a plausible CO2/H2O-dominated atmosphere demonstrate the potential for effective greenhouse warming.[16] These models highlight the planet's sensitivity to atmospheric thickness and composition, where modest volatile inventories akin to Earth's could prevent freezing despite the subdued stellar input. A 2025 reassessment of Kepler habitable zone candidates using data-driven null-signal templates assigned Kepler-186f a 20% false alarm probability, suggesting its detection may be marginal.[2] As of November 2025, archival James Webb Space Telescope data provides no direct imaging or spectroscopic detection for Kepler-186f owing to the system's distance and faintness. Transit observations of analogous habitable-zone rocky planets orbiting M dwarfs have established stringent upper limits on extended H/He envelopes, typically constraining such atmospheres to less than 10% of the planet's total mass.[21] These constraints favor thinner, secondary atmospheres more conducive to habitability over primordial gas layers that would otherwise drive excessive heat retention or loss.

Broader implications

The discovery of Kepler-186f in 2014 marked a significant milestone in exoplanet research, as it was the first validated planet with a radius smaller than 1.5 times that of Earth located within the habitable zone of its host star.[22] This finding, based on transit photometry data from NASA's Kepler mission, demonstrated that Earth-sized worlds capable of potentially supporting liquid water exist around cool stars other than the Sun.[22] The Kepler-186 system has contributed to refined estimates of planet occurrence rates around M dwarfs, informing broader statistical models of habitable worlds in the galaxy. Analysis of Kepler data indicates that approximately 0.16 to 0.24 Earth-sized planets (1–1.5 Earth radii) per M dwarf reside in conservative to broader habitable zones, highlighting the prevalence of such systems despite detection biases.[23] Observing Kepler-186f's atmosphere poses substantial challenges for current and near-future telescopes due to the system's distance of about 580 light-years and the host star's faint apparent magnitude of around 15.3 in the V-band, which limits signal-to-noise ratios for transmission spectroscopy.[3] The James Webb Space Telescope (JWST) faces difficulties in characterizing atmospheres of Earth-sized planets around such distant M dwarfs, as the transit depth signals are marginal even in the near-infrared. However, ground-based extremely large telescopes like the ELT offer potential for high-resolution cross-correlation spectroscopy to detect molecular features, providing complementary follow-up opportunities for nearby to moderately distant habitable candidates.[24] In astrobiology contexts, planets like Kepler-186f in the habitable zones of M dwarfs have served as benchmarks for modeling biosignature detectability, with studies simulating atmospheric compositions featuring disequilibrium pairs like methane and oxygen to assess habitability indicators under M-dwarf stellar radiation. These models emphasize challenges such as photochemical destruction and false positives but underscore the role of such planets in testing observational strategies for life detection. Radio searches targeting the system, including observations with the Allen Telescope Array in 2014, have yielded no technosignature signals; no subsequent detections have been reported as of November 2025.[25]
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