Astronomy:Kilodegree Extremely Little Telescope

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Kilodegree Extremely Little Telescope
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The Kilodegree Extremely Little Telescope (or KELT) is an astronomical observation system formed by two robotic telescopes that are conducting a survey for transiting exoplanets around bright stars. The project is jointly administered by members of Ohio State University Department of Astronomy,[1] the Vanderbilt University Department of Physics and Astronomy[2] Astronomy Group,[3] the Lehigh University Department of Physics,[4] and the South African Astronomical Observatory (SAAO).[5]

KELT Telescopes

KELT consists of two telescopes, KELT-North[6] in Arizona in the United States, and KELT-South[7] at the SAAO observing station near Sutherland, South Africa.

Each KELT telescope consists of a wide field (26 degrees × 26 degrees) medium format telephoto lens with a 4.2 cm aperture, mounted in front of a 4k × 4k Apogee CCD. Each can also be equipped with an alternative narrower field (10.8 degrees × 10.8 degrees) lens with a 7.1 cm aperture for a narrow angle campaign mode. KELT-North uses an Apogee AP16E camera, while KELT South uses an Apogee U16M. The optical assemblies and cameras are mounted on Paramount ME[8] mounts manufactured by Software Bisque.[9] The telescopes were made with off-the-shelf components, and were thus much cheaper than many observatories.[10]

  • KELT-North is located at Winer Observatory in southeastern Arizona, about an hour's drive from Tucson. KELT-North was installed at Winer in 2005, and operated continuously until 2022, with occasional interruptions for equipment failures and poor weather. KELT-North was decommissioned in 2022.
  • KELT-South is located at the Sutherland astronomical observation station owned and operated by SAAO, about 370 kilometers (230 mi) North of Cape Town. KELT-South was deployed at Sutherland in 2009.

Goals

KELT is dedicated to discovering transiting exoplanets orbiting stars in the apparent magnitude range of 8 < V < 10. This is the region just fainter than the set of stars comprehensively surveyed for planets by the radial-velocity surveys, but brighter than those typically observed by most transit surveys.

Operations

Both KELT telescopes operate by sequentially observing a series of predefined fields around the sky all night, every night when the weather is good. All recordings are made with 150-second exposures, optimized to observe stars in the target magnitude range.

Discoveries

KELT has made several exoplanet discoveries and at least one brown dwarf (which may be an extremely massive Super-Jupiter instead) to date. Yellow rows in the table below indicate the planet is contained in a binary system.

Exoplanets

Star Constellation Right
ascension 		Declination App.
mag. 		Distance (ly) Spectral
type 		Planet Mass
(MJ) 		Radius
(RJ) 		Density
(g/cm3) 		Orbital
period
(d) 		Semimajor
axis
(AU) 		Orbital
eccentricity 		Inclination
(°) 		Discovery
year
KELT-2A Auriga  06h 10m 39s +30° 57′ 26″ 8.77 420 F7V KELT-2Ab 1.486 1.306 4.11379 0.05498 0.0 88.5 2012
KELT-3 Leo  09h 54m 34.0s +30° 38′ 24″ 9.8 580 F6V KELT-3b 1.418 1.333 0.75 2.70339 0.04117 0.0 84.32 2012
KELT-4A Leo  10h 28m 15.011s +25° 34′ 23.5″ 9.98 685 F8V KELT-4Ab 0.878 1.706 2.9895933 0.04321 0.0 83.11 2015
KELT-6 Coma Berenices  13h 03m 56s +30° 38′ 24″ 10.38 724 F8IV KELT-6b 0.43 1.19 0.311 7.84563 0.079 0.22 +0.12−0.10 88.81 2013
KELT-6c 3.71 1.16 1,276 2.39 0.21 2015
KELT-7 Auriga  05h 13m 11s +33° 19′ 05″ 8.54 420 F2V KELT-7b 1.28 1.533 0.442 2.7347749 0.04415 0.0 83.76 2015
KELT-8 Hercules  18h 53m 13.31s 24° 07′ 38.09″ 10.85 664 G2V KELT-8b 0.66 1.62 0.165 3.24 0.04550 0.04±0.05 82.65±0.90 2015
KELT-9 Cygnus  20h 31m 27s +39° 56′ 20″ 7.56 620 B9.5V KELT-9b 2015
KELT-10 Telescopium  18h 58m 11.61s −47° 00′ 11.91″ 10.62 614 G0V KELT-10b 0.68 1.4 0.308 4.17 0.05250 0? 88.61 2015
KELT-11 Sextans  10h 46m 49.66s −09° 23′ 57.71″ 8.04 323 G8/K0IV KELT-11b 0.171 1.35 0.009 4.74 0.06±0.005 0.0007±0.0015 85.3±0.2 2017
KELT-12 Hercules  17h 50m 33.72s +36° 34′ 12.63″ 10.59 1200 F7III-IV KELT-12b 0.95 1.78 0.209 5.03 0.06708 0.0 84.47±0.15 2017
KELT-13/WASP-167 Centaurus  13h 04m 10.51s −35° 32′ 58.31″ 10.571 1381 F1V KELT-13/WASP-167b <8 1.58 2.02 0.0365 79.9 2017
KELT-14/WASP-122 Puppis  7h 13m 12.34s −42° 24′ 35.14″ 11 816 G2V KELT-14/WASP-122b 1.284 1.743 0.322 1.71 0.03 0.0 78.3 2016
KELT-15 Carina  07h 49m 39.59s −52° 07′ 13.57″ 11.39 1,068 G0V KELT-15Ab 0.91 1.443 0.36 3.33 0.04 0 88.3 2015
KELT-16 Cygnus  20h 57m 04.44s +31° 39′ 39.63″ 11.72 1,469 F7V KELT-16Ab[11] 2.75 1.415 1.20 ± 0.18 0.97 0.02 0 84.4 2017
KELT-17 Cancer  8h 22m 28.20s +13° 44′ 07.14″ 9.23 743 A7V KELT-17b 1.32 1.525 0.46 3.08 0.05 84.87 2016
KELT-18 Ursa Major  14h 26m 05.76s +59° 26′ 39.29″ 10.16 1,057 F4V KELT-18Ab[12] 1.18 1.57 0.377 2.87 0.04 0 82.90 2017
KELT-19 Canis Minor  07h 26m 02.29s +07° 36′ 56.18″ 9.86 987 A8V KELT-19Ab <4.07 1.91 <0.744 4.61 0.064 85.14 2017
KELT-20 Cygnus  19h 38m 38.74s +31° 31′ 09.22″ 7.58 446 A2V KELT-20b <3.382 1.741 <0.806 3.474 0.05 0? 86.12 2017
KELT-21 Cygnus  20h 19m 12.00s +32° 34′ 51.76″ 10.48 1,556 A6V KELT-21b <3.91 1.586 <1.24 3.612 0.05 0 86.46 2018
KELT-22/WASP-173 Sculptor  23h 36m 40.38s −34° 36′ 42.68″ 11.3 766 G3V KELT-22/WASP-173Ab 3.47 1.285 2.02 1.386 0.02 0 85.2 2018
KELT-23 Ursa Minor  15h 28m 35.19s +66° 21′ 31.54″ 10.31 413 G1V KELT-23b 0.94 1.32 0.503 2.26 0.03 0 85.37 2019
KELT-24 Ursa Major  10h 47m 38.35s +71° 39′ 21.16″ 8.33 316 F5.5V KELT-24b 5.18 1.27 3.13 5.55 0.07 0.08 89.17 2019
KELT-25 Canis Major  07h 12m 29.55s −24° 57′ 12.82″ 9.63 1,443 A4V
KELT-26/WASP-178 Lupus  15h 09m 04.89s −42° 42′ 17.79″ 9.95 1,410 A1V KELT-26/WASP-178b 1.41 1.94 0.238 3.35 0.06 0 84.45 2019

Brown dwarfs

In addition, the survey has discovered brown dwarfs like KELT-1b.

Star Constellation Right
ascension 		Declination App.
mag. 		Distance (ly) Spectral
type 		Planet Mass
(MJ) 		Radius
(RJ) 		Density
(g/cm3) 		Orbital
period
(d) 		Semimajor
axis
(AU) 		Orbital
eccentricity 		Inclination
(°) 		Discovery
year
KELT-1 Andromeda  00h 01m 26.92s +39° 23′ 01.7″ 10.00 854 F5V KELT-1b 27.23 1.110 1.217513 0.0247 0.0 87.80

References

  1. ↑ "The Ohio State University Department of Astronomy". http://astronomy.osu.edu. 
  2. ↑ "Vanderbilt Department of Physics and Astronomy". http://www.vanderbilt.edu/physics/. 
  3. ↑ "Vanderbilt Astronomy Group". http://as.vanderbilt.edu/astronomy/. 
  4. ↑ "The Lehigh Department of Physics". http://physics.cas2.lehigh.edu/. 
  5. ↑ "South African Astronomical Observatory". http://www.saao.ac.za/. 
  6. ↑ Pepper, Joshua et al. (2007). "The Kilodegree Extremely Little Telescope (KELT): A Small Robotic Telescope for Large-Area Synoptic Surveys". Publications of the Astronomical Society of the Pacific 119 (858): 923–935. doi:10.1086/521836. Bibcode: 2007PASP..119..923P. 
  7. ↑ Pepper (2012). "The KELT-South Telescope". Publications of the Astronomical Society of the Pacific 124 (913): 230–241. doi:10.1086/665044. Bibcode: 2012PASP..124..230P. 
  8. ↑ "Paramount ME". Archived from the original on 2012-07-02. https://web.archive.org/web/20120702172826/http://www.bisque.com/sc/pages/Paramount-ME.aspx. 
  9. ↑ "Software Bisque company page". http://www.bisque.com. 
  10. ↑ Sample, Ian (2017-06-05). "Kelt-9b: astronomers discover hottest known giant planet" (in en-GB). The Guardian. ISSN 0261-3077. https://www.theguardian.com/science/2017/jun/05/kelt-9b-astronomers-discover-hottest-known-giant-planet. 
  11. ↑ Oberst, Thomas E.; Rodriguez, Joseph E.; Colón, Knicole D.; Angerhausen, Daniel; Bieryla, Allyson; Ngo, Henry; Stevens, Daniel J.; Stassun, Keivan G. et al. (2017). "KELT-16b: A Highly Irradiated, Ultra-short Period Hot Jupiter Nearing Tidal Disruption". The Astronomical Journal 153 (3): 97. doi:10.3847/1538-3881/153/3/97. Bibcode: 2017AJ....153...97O. 
  12. ↑ McLeod, Kim K.; Rodriguez, Joseph E.; Oelkers, Ryan J.; Collins, Karen A.; Bieryla, Allyson; Fulton, Benjamin J.; Stassun, Keivan G.; Gaudi, B. Scott et al. (2017). "KELT-18b: Puffy Planet, Hot Host, Probably Perturbed". The Astronomical Journal 153 (6): 263. doi:10.3847/1538-3881/aa6d5d. Bibcode: 2017AJ....153..263M. 

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