From 9d1c060883d638c7e8077a4e9130770b51b9309e Mon Sep 17 00:00:00 2001 From: turtle89431 Date: Tue, 5 May 2026 02:41:13 -0700 Subject: [PATCH] Scrape wikipedia-science: 5665 new, 3147 updated, 9073 total (kb-cron) --- _index.db | Bin 78934016 -> 79040512 bytes data/en.wikipedia.org/wiki/ARCADE-0.md | 35 ++++ .../wiki/ARGOS_(optics_system)-0.md | 15 ++ .../en.wikipedia.org/wiki/Active_surface-0.md | 26 +++ data/en.wikipedia.org/wiki/Alidade-0.md | 2 +- data/en.wikipedia.org/wiki/Almucantar-0.md | 2 +- .../wiki/Antikythera_mechanism-0.md | 2 +- .../wiki/Antikythera_mechanism-1.md | 2 +- .../wiki/Antikythera_mechanism-10.md | 2 +- .../wiki/Antikythera_mechanism-11.md | 2 +- .../wiki/Antikythera_mechanism-2.md | 2 +- .../wiki/Antikythera_mechanism-3.md | 2 +- .../wiki/Antikythera_mechanism-4.md | 2 +- .../wiki/Antikythera_mechanism-5.md | 2 +- .../wiki/Antikythera_mechanism-6.md | 2 +- .../wiki/Antikythera_mechanism-7.md | 2 +- .../wiki/Antikythera_mechanism-8.md | 2 +- 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z8u0B}!Vyr#>3OjXJsc0dfBGwUw8aTl$8XiOvwpCtHuKs8IlwBpV{!Iwj@Hm0=RK!4 z`NF7|CPH?JLsRph)2(iCQVW-|iNx5qY#uyzwF=L3y@`Orx>rZmz}3sCWNZ)Mc;$4a z!!O2BCDEKU*vWzZGzTQp*d$anCM!uiZt^slQA{8=We#x7>j;lHwMEjY&fztg{W_Rg zbfIz9fRk7r*oW{H>N|qwY$0}fR6xo$_Z=%otiufsSsIgk2u~BdrVJC(wPoJtjMAWi z;kDH=Ax>40IB~xL0Et6QFc&z}1izu2Ybmvt(XNSX%H^vinPu~(1F-EDo@a5f#dMmL oevJzdF-%IW3%orVI=XiOe-NOWN`T_0J3%)tl)+@mHJJ1N2Rhzis{jB1 diff --git a/data/en.wikipedia.org/wiki/ARCADE-0.md b/data/en.wikipedia.org/wiki/ARCADE-0.md new file mode 100644 index 000000000..e4688595c --- /dev/null +++ b/data/en.wikipedia.org/wiki/ARCADE-0.md @@ -0,0 +1,35 @@ +--- +title: "ARCADE" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/ARCADE" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:00.350251+00:00" +instance: "kb-cron" +--- + +Absolute Radiometer for Cosmology, Astrophysics, and Diffuse Emission (ARCADE) is a program which utilizes high-altitude balloon instrument package intended to measure the heating of the universe by the first stars and galaxies after the big bang and search for the signal of relic decay or annihilation. In July 2006 a strong residual radio source was found using the radiometer, approximately six times what is predicted by theory. This phenomenon is known as "space roar" and remains an unsolved problem in astrophysics. + +ARCADE has been funded by the NASA's Science Mission Directorate under the Astronomy and Physics Research and Analysis Suborbital Investigation program. The program is composed of a team led by Alan Kogut of NASA's Goddard Space Flight Center. ARCADE was launched from NASA's Columbia Scientific Balloon Facility in Palestine, Texas, conducted under the auspices of the Balloon Program Office at Wallops Flight Facility. The balloon flew to an altitude of 120,000 feet (37 km), viewing about 7% of the sky during its observations. +The instrument is designed to detect radiation at centimeter wavelengths. The craft contained seven radiometers which were cooled to 2.7 K (−270.45 °C; −454.81 °F) using liquid helium, with the intent to measure temperature differences as small as 1/1000 of a degree against a background which is only 3 K (−270.15 °C; −454.27 °F). The optics in the instrument package were placed near the top of the dewar flask which cooled them in order to prevent the instruments from seeing the walls of the container, thereby simplifying the processing of the observational data. This design choice necessitated the use of superfluid pumps in order to drench the radiometers in liquid helium. The design also utilized heaters in order to create a cloud of helium gas, in place of using a (relatively warm) window, which also simplified processing of the observational data. + + +== Residual emission == +In 2011, the ARCADE 2 researchers reported, "Correcting for instrumental systematic errors in measurements such as ARCADE 2 is always a primary concern. We emphasize that we detect residual emission at 3 GHz with the ARCADE 2 data, but the result is also independently detected by a combination of low-frequency data and FIRAS." +The ARCADE 2 science team came to the following conclusion concerning the unexpected residual emission at 3 GHz: + +We conclude that the residual signature is due either to a diffuse extragalactic background of emission from discrete radio sources with properties somewhat different than the faint end of the distribution of known sources or to unmodeled residual emission from our own Galaxy. Although we believe the former to be more likely, we cannot exclude the latter explanation. +Radio waves have frequencies from 30 Hz to 300 GHz. The term space roar has been used to indicate the hypothesis that the ARCADE 2 results indicate that the actual faint end of the emission distribution of known sources is significantly different from the expected value predicted by the Lambda-CDM model given the known sources of emission. Possible hypothetical sources include diffuse large-scale turbulently merging clusters of galaxies or supernovae of the primary generations of stars. + + +== See also == + +List of cosmic microwave background experiments +Cosmic microwave background radiation + + +== References == + + +== External links == +NASA's ARCADE Archived 2012-02-20 at the Wayback Machine \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/ARGOS_(optics_system)-0.md b/data/en.wikipedia.org/wiki/ARGOS_(optics_system)-0.md new file mode 100644 index 000000000..aa043c3fa --- /dev/null +++ b/data/en.wikipedia.org/wiki/ARGOS_(optics_system)-0.md @@ -0,0 +1,15 @@ +--- +title: "ARGOS (optics system)" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/ARGOS_(optics_system)" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:02.754542+00:00" +instance: "kb-cron" +--- + +Advanced Rayleigh Guided Ground Layer Adaptive Optics System (ARGOS) is a multi-star adaptive optics system which is built for use with the Large Binocular Telescope (LBT). +With ARGOS, both sides of the LBT will be equipped with a multi-laser beacon system and corresponding wavefront sensors. The artificial beacons are created by Rayleigh scattering the Earth's atmosphere using high power pulsed green lasers. The purpose of ARGOS is to generate six artificial laser guides stars to correct the ground layer turbulence above the LBT mirrors. This will decrease the distortions induced by the atmospheric turbulence, and therefore the imaging and spectroscopic capability of LUCIFER, the LBT spectrograph. + + +== References == \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Active_surface-0.md b/data/en.wikipedia.org/wiki/Active_surface-0.md new file mode 100644 index 000000000..10c833b3c --- /dev/null +++ b/data/en.wikipedia.org/wiki/Active_surface-0.md @@ -0,0 +1,26 @@ +--- +title: "Active surface" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Active_surface" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:39:55.307901+00:00" +instance: "kb-cron" +--- + +An active surface is a surface of a radio telescope that is under active computer control of its shape. +Large radio telescopes (more than 10 m in diameter or length) always bend during operation, due to their enormous weight and the fact that even the strongest materials are not perfectly stiff. This bending, in the range of a few millimetres, does not affect low frequency operation much, but dramatically reduces the efficiency of the telescope at higher frequencies where the wavelengths are comparable to the distortion. Typically, the efficiency of a telescope drops appreciably when the deviation from the desired shape is more than 1/10 of the considered wavelength. An active surface uses numerous small actuators to move the surface panels with respect to the underlying frame, and thus maintain the correct shape. +An active surface can try to compensate for many different types of errors. The first is gravity—this is simplest since previous measurements, or even a mathematical model, can be used to predict (and correct) any bending. More difficult is correction for wind and thermal errors, since these require measuring and correcting in real time. +Some examples of active surfaces are: + +Green Bank Telescope +Large Millimeter Telescope +Sardinia Radio Telescope +Noto Radio Observatory +The Chinese Five hundred meter Aperture Spherical Telescope uses a uniquely ambitious form of active surface, not only correcting errors, but applying deflections of up to 47 centimetres (19 in) in order to aim and focus the telescope. + + +== References == +Parker, D.H. & Payne, J.M. (2002). "Active Surface Architectures of Large Radio Telescopes" (PDF). International Union of Radio Science (URSI) XXVII General Assembly, Maastricht, The Netherlands. Archived from the original (PDF) on 2011-05-22. Retrieved 2008-10-24. +Orfel, A.; Morsiani, M.; Zacchiroli, G.; Maccaferri, G.; Roda, J. & Fiocchi, F. (2004). "An active surface for large reflector antennas". IEEE Transactions on Antennas and Propagation. 46 (4): 11–19. Bibcode:2004IAPM...46...11O. doi:10.1109/MAP.2004.1373995. S2CID 42428849.. Discusses many practical details of an active surface. +Normile, Dennis (26 September 2016). "World's largest radio telescope will search for dark matter, listen for aliens". Science News. doi:10.1126/science.aah7346. \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Alidade-0.md b/data/en.wikipedia.org/wiki/Alidade-0.md index 39b3d42a6..370771464 100644 --- a/data/en.wikipedia.org/wiki/Alidade-0.md +++ b/data/en.wikipedia.org/wiki/Alidade-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Alidade" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:20.541498+00:00" +date_saved: "2026-05-05T09:39:56.566183+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Almucantar-0.md b/data/en.wikipedia.org/wiki/Almucantar-0.md index 4be62f2f0..28ebd2465 100644 --- a/data/en.wikipedia.org/wiki/Almucantar-0.md +++ b/data/en.wikipedia.org/wiki/Almucantar-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Almucantar" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:21.691077+00:00" +date_saved: "2026-05-05T09:39:57.899944+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Antikythera_mechanism-0.md b/data/en.wikipedia.org/wiki/Antikythera_mechanism-0.md index 4a6381a00..14e84bb59 100644 --- a/data/en.wikipedia.org/wiki/Antikythera_mechanism-0.md +++ b/data/en.wikipedia.org/wiki/Antikythera_mechanism-0.md @@ -4,7 +4,7 @@ chunk: 1/12 source: "https://en.wikipedia.org/wiki/Antikythera_mechanism" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T06:22:49.894379+00:00" +date_saved: "2026-05-05T09:39:59.175186+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Antikythera_mechanism-1.md b/data/en.wikipedia.org/wiki/Antikythera_mechanism-1.md index 2073f3a48..94b7f0d5b 100644 --- a/data/en.wikipedia.org/wiki/Antikythera_mechanism-1.md +++ b/data/en.wikipedia.org/wiki/Antikythera_mechanism-1.md @@ -4,7 +4,7 @@ chunk: 2/12 source: "https://en.wikipedia.org/wiki/Antikythera_mechanism" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T06:22:49.894379+00:00" +date_saved: "2026-05-05T09:39:59.175186+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Antikythera_mechanism-10.md b/data/en.wikipedia.org/wiki/Antikythera_mechanism-10.md index 86e034028..dc0e9f2a5 100644 --- a/data/en.wikipedia.org/wiki/Antikythera_mechanism-10.md +++ b/data/en.wikipedia.org/wiki/Antikythera_mechanism-10.md @@ -4,7 +4,7 @@ chunk: 11/12 source: "https://en.wikipedia.org/wiki/Antikythera_mechanism" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T06:22:49.894379+00:00" +date_saved: "2026-05-05T09:39:59.175186+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Antikythera_mechanism-11.md b/data/en.wikipedia.org/wiki/Antikythera_mechanism-11.md index c40f57fed..685b7f504 100644 --- a/data/en.wikipedia.org/wiki/Antikythera_mechanism-11.md +++ b/data/en.wikipedia.org/wiki/Antikythera_mechanism-11.md @@ -4,7 +4,7 @@ chunk: 12/12 source: "https://en.wikipedia.org/wiki/Antikythera_mechanism" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T06:22:49.894379+00:00" +date_saved: "2026-05-05T09:39:59.175186+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Antikythera_mechanism-2.md b/data/en.wikipedia.org/wiki/Antikythera_mechanism-2.md index eb65318fd..b962fbf3c 100644 --- a/data/en.wikipedia.org/wiki/Antikythera_mechanism-2.md +++ b/data/en.wikipedia.org/wiki/Antikythera_mechanism-2.md @@ -4,7 +4,7 @@ chunk: 3/12 source: "https://en.wikipedia.org/wiki/Antikythera_mechanism" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T06:22:49.894379+00:00" +date_saved: "2026-05-05T09:39:59.175186+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Antikythera_mechanism-3.md b/data/en.wikipedia.org/wiki/Antikythera_mechanism-3.md index 7c5adf99a..ea4ecf657 100644 --- a/data/en.wikipedia.org/wiki/Antikythera_mechanism-3.md +++ b/data/en.wikipedia.org/wiki/Antikythera_mechanism-3.md @@ -4,7 +4,7 @@ chunk: 4/12 source: "https://en.wikipedia.org/wiki/Antikythera_mechanism" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T06:22:49.894379+00:00" +date_saved: "2026-05-05T09:39:59.175186+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Antikythera_mechanism-4.md b/data/en.wikipedia.org/wiki/Antikythera_mechanism-4.md index d0da64622..bb5bd248e 100644 --- a/data/en.wikipedia.org/wiki/Antikythera_mechanism-4.md +++ b/data/en.wikipedia.org/wiki/Antikythera_mechanism-4.md @@ -4,7 +4,7 @@ chunk: 5/12 source: "https://en.wikipedia.org/wiki/Antikythera_mechanism" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T06:22:49.894379+00:00" +date_saved: "2026-05-05T09:39:59.175186+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Antikythera_mechanism-5.md b/data/en.wikipedia.org/wiki/Antikythera_mechanism-5.md index 0ba95ce85..b7c7b486b 100644 --- a/data/en.wikipedia.org/wiki/Antikythera_mechanism-5.md +++ b/data/en.wikipedia.org/wiki/Antikythera_mechanism-5.md @@ -4,7 +4,7 @@ chunk: 6/12 source: "https://en.wikipedia.org/wiki/Antikythera_mechanism" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T06:22:49.894379+00:00" +date_saved: "2026-05-05T09:39:59.175186+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Antikythera_mechanism-6.md b/data/en.wikipedia.org/wiki/Antikythera_mechanism-6.md index ae88b0e8b..4de119bc7 100644 --- a/data/en.wikipedia.org/wiki/Antikythera_mechanism-6.md +++ b/data/en.wikipedia.org/wiki/Antikythera_mechanism-6.md @@ -4,7 +4,7 @@ chunk: 7/12 source: "https://en.wikipedia.org/wiki/Antikythera_mechanism" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T06:22:49.894379+00:00" +date_saved: "2026-05-05T09:39:59.175186+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Antikythera_mechanism-7.md b/data/en.wikipedia.org/wiki/Antikythera_mechanism-7.md index ac0c7bec9..c7db571f5 100644 --- a/data/en.wikipedia.org/wiki/Antikythera_mechanism-7.md +++ b/data/en.wikipedia.org/wiki/Antikythera_mechanism-7.md @@ -4,7 +4,7 @@ chunk: 8/12 source: "https://en.wikipedia.org/wiki/Antikythera_mechanism" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T06:22:49.894379+00:00" +date_saved: "2026-05-05T09:39:59.175186+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Antikythera_mechanism-8.md b/data/en.wikipedia.org/wiki/Antikythera_mechanism-8.md index 0bf239488..5ea421ef7 100644 --- a/data/en.wikipedia.org/wiki/Antikythera_mechanism-8.md +++ b/data/en.wikipedia.org/wiki/Antikythera_mechanism-8.md @@ -4,7 +4,7 @@ chunk: 9/12 source: "https://en.wikipedia.org/wiki/Antikythera_mechanism" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T06:22:49.894379+00:00" +date_saved: "2026-05-05T09:39:59.175186+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Antikythera_mechanism-9.md b/data/en.wikipedia.org/wiki/Antikythera_mechanism-9.md index d8f726c57..d0eb32f89 100644 --- a/data/en.wikipedia.org/wiki/Antikythera_mechanism-9.md +++ b/data/en.wikipedia.org/wiki/Antikythera_mechanism-9.md @@ -4,7 +4,7 @@ chunk: 10/12 source: "https://en.wikipedia.org/wiki/Antikythera_mechanism" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T06:22:49.894379+00:00" +date_saved: "2026-05-05T09:39:59.175186+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Archeops-0.md b/data/en.wikipedia.org/wiki/Archeops-0.md new file mode 100644 index 000000000..5094fc9b4 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Archeops-0.md @@ -0,0 +1,32 @@ +--- +title: "Archeops" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Archeops" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:01.559118+00:00" +instance: "kb-cron" +--- + +Archeops was a balloon-borne instrument dedicated to measuring the Cosmic microwave background (CMB) temperature anisotropies. The study of this radiation is essential to obtain precise information on the evolution of the Universe: density, Hubble constant, age of the Universe, etc. To achieve this goal, measurements were done with devices cooled down at 100mK temperature placed at the focus of a warm telescope. To avoid atmospheric disturbance the whole apparatus is placed on a gondola below a helium balloon that reaches 40 km altitude. +Archeops has four bands in the millimeter domain (143, 217, 353 and 545 GHz) with a high angular resolution (about 15 arcminutes) in order to constrain small anisotropy scales, as well as a large sky coverage fraction (30%) in order to minimize the intrinsic cosmic variance. + + +== Instrument and flights == +The instrument was designed by adapting concepts put forward for the High Frequency Instrument of Planck surveyor (Planck-HFI) and using balloon-borne constraints. +Namely, it consists of an open 3He-4He dilution cryostat cooling spiderweb-type bolometers at 100 mK; cold individual optics with horns at different temperature stages (0.1, 1.6, 10 K) and an off-axis Gregorian telescope. +The CMB signal is measured by the 143 and 217 GHz detectors while interstellar dust emission and atmospheric emission are monitored with the 353 (polarized) and 545 GHz detectors. +The whole instrument is baffled so as to avoid stray radiation from the Earth and the balloon. +To cover as far as 30% of the sky, the payload was spinning mostly above the atmosphere, scanning the sky in circles with a fixed elevation of roughly 41 degrees. The gondola, at a float altitude above 32 km, spins across the sky at a rate of 2 rpm which, combined with the Earth rotation, produces a well sampled sky at each frequency. +Archeops flew for the first time in Trapani (Sicily) with four–hours integration time. Then, the upgraded instrument was launched three times from the Esrange base near Kiruna (Sweden) by the CNES during 2 consecutive Winter seasons (2001 and 2002). The last and best flight on Feb. 7th, 2002 yields 12.5 hours of CMB–type data (at ceiling altitude and by night) from a 19–hours total. The balloon landed in Siberia and it was recovered (with its precious data recorded on–board) by a Franco–Russian team with −40 °C weather. + + +== Results == + +Archeops has linked, for the first time and before WMAP, the large angular scales (previously measured by COBE) to the first acoustic peak region. +From its results, inflation motivated cosmologies have been reinforced with a flat Universe (total energy density Ωtot = 1 within 3%). +When combined with complementary cosmological datasets regarding the value of Hubble's constant, Archeops gives constraints on the dark energy density and the baryonic density in very good agreement with other independent estimations based on supernovae measurements and big bang nucleosynthesis. +Archeops has given the first polarized maps of the galactic dust emission with this resolution. + + +== References == \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Armillary_sphere-0.md b/data/en.wikipedia.org/wiki/Armillary_sphere-0.md index 9ba9c7d2e..0b292a6bc 100644 --- a/data/en.wikipedia.org/wiki/Armillary_sphere-0.md +++ b/data/en.wikipedia.org/wiki/Armillary_sphere-0.md @@ -4,7 +4,7 @@ chunk: 1/5 source: "https://en.wikipedia.org/wiki/Armillary_sphere" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:22.848952+00:00" +date_saved: "2026-05-05T09:40:04.003517+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Armillary_sphere-1.md b/data/en.wikipedia.org/wiki/Armillary_sphere-1.md index 3f1f4b2ab..e23c49976 100644 --- a/data/en.wikipedia.org/wiki/Armillary_sphere-1.md +++ b/data/en.wikipedia.org/wiki/Armillary_sphere-1.md @@ -4,7 +4,7 @@ chunk: 2/5 source: "https://en.wikipedia.org/wiki/Armillary_sphere" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:22.848952+00:00" +date_saved: "2026-05-05T09:40:04.003517+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Armillary_sphere-2.md b/data/en.wikipedia.org/wiki/Armillary_sphere-2.md index 177373b51..7f4d6410b 100644 --- a/data/en.wikipedia.org/wiki/Armillary_sphere-2.md +++ b/data/en.wikipedia.org/wiki/Armillary_sphere-2.md @@ -4,7 +4,7 @@ chunk: 3/5 source: "https://en.wikipedia.org/wiki/Armillary_sphere" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:22.848952+00:00" +date_saved: "2026-05-05T09:40:04.003517+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Armillary_sphere-3.md b/data/en.wikipedia.org/wiki/Armillary_sphere-3.md index e8dedfd75..3282910e1 100644 --- a/data/en.wikipedia.org/wiki/Armillary_sphere-3.md +++ b/data/en.wikipedia.org/wiki/Armillary_sphere-3.md @@ -4,7 +4,7 @@ chunk: 4/5 source: "https://en.wikipedia.org/wiki/Armillary_sphere" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:22.848952+00:00" +date_saved: "2026-05-05T09:40:04.003517+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Armillary_sphere-4.md b/data/en.wikipedia.org/wiki/Armillary_sphere-4.md index a0635d9c4..027a8cc92 100644 --- a/data/en.wikipedia.org/wiki/Armillary_sphere-4.md +++ b/data/en.wikipedia.org/wiki/Armillary_sphere-4.md @@ -4,7 +4,7 @@ chunk: 5/5 source: "https://en.wikipedia.org/wiki/Armillary_sphere" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:22.848952+00:00" +date_saved: "2026-05-05T09:40:04.003517+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Astrarium-0.md b/data/en.wikipedia.org/wiki/Astrarium-0.md index 4965db091..d79259d10 100644 --- a/data/en.wikipedia.org/wiki/Astrarium-0.md +++ b/data/en.wikipedia.org/wiki/Astrarium-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Astrarium" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:25.196479+00:00" +date_saved: "2026-05-05T09:40:05.273096+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Astrograph-0.md b/data/en.wikipedia.org/wiki/Astrograph-0.md new file mode 100644 index 000000000..e94d66969 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Astrograph-0.md @@ -0,0 +1,55 @@ +--- +title: "Astrograph" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Astrograph" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:06.451632+00:00" +instance: "kb-cron" +--- + +An astrograph (or astrographic camera) is a telescope designed for the sole purpose of astrophotography. Astrographs are mostly used in wide-field astronomical surveys of the sky and for detection of objects such as asteroids, meteors, and comets. +Improvements in photography in the middle 19th century led to designs dedicated to astrophotography, and they were also popular in the 20th century. As in other photography, chemicals were used that respond to light, recorded on a glass photographic plate or sometimes on photographic film. Many observatories of this period used an astrograph, beside instruments like the transit telescope, great refractors, and chronometers, or instruments for observing the Sun. +Astrographs were often used to make surveys of the night sky, and one of the famous projects was Carte du Ciel. Discoveries using an astrograph include then-planet Pluto. Rather than looking through the telescope, it was discovered by using a blink comparator with images taken by an astrograph. +By the late 20th century, electronic detectors became more common with the data being stored electronically. + + +== Design == +Most research telescopes in this class are refractors, although there are many (usually larger) reflecting designs such as the Ritchey-Chrétien and catadioptrics such as the Schmidt camera. The main parameters of an Astrograph are the diameter and f-ratio of the objective, which determine the field of view and image scale on the photographic plate or CCD detector. The objective of an astrograph is usually not very large, on the order of 20 to 50 cm (8 to 20 in). +The shape of the focal plane is often designed to work in conjunction with a specific shaped photographic plate or CCD detector. The objective is designed to produce a particularly large (for example, 17 by 17 inches (430 mm × 430 mm)), flat, and distortionless image at the focal plane. They may even be designed to focus certain wavelengths of light to match the type of film they are designed to use (early astrographs were corrected to work in blue wavelengths to match photographic emulsions of the time). +Wide-angle astrographs with short f-ratios are used for photographing a huge area of sky. Astrographs with higher f-ratios are used in more precise measurements. Many observatories of the world are equipped with the so-called normal astrographs with an aperture of around 13 inches (330 mm) and a focal length of 11 feet (3.4 m). The purpose of a "normal astrograph" is to create images where the scale of the image at the focal plane is a standard of approximately 60 arcsecs/mm. + + +== Applications == + + +=== Astrometry === +Astrographs used in astrometry record images that are then used to "map" the positions of objects over a large area of the sky. These maps are then published in catalogs to be used in further study or to serve as reference points for deep-space imaging. + + +=== Stellar classification === +Astrographs used for stellar classification sometimes consist of two identical telescopes on the same mount (a double astrograph). Each sky field can be simultaneously photographed in two colors (usually blue and yellow). Each telescope may have individually designed non-achromatic objectives to focus the desired wavelength of light which is paired with the respective color-sensitive (black-and-white) photographic plate. In other cases a single telescope is used to make two exposures of the same part of the sky with different filters and color sensitive film used on each exposure. Two-color photography lets astronomers measure the color, as well as the brightness (magnitude), of each star imaged. Colors tell the star's "temperature". Knowing the color type and magnitudes lets astronomers determine the distance of a star. Sky fields that are photographed twice, decades apart in time, will reveal a nearby star's proper motion when measured against the background of distant stars or galaxies. + + +=== Discovery of astronomical objects === +By taking two exposures of the same section of the sky days or weeks apart, it is possible to find objects such as asteroids, meteors, comets, variable stars, novae, and even unknown planets. By comparing the pair of images, using a device such as a blink comparator, astronomers are able to find objects that moved or changed brightness between the two exposures or simply appear in one image only, as in the case of a nova or meteor. Sometimes objects can even be found in one exposure since a fast moving object will appear as a "line" in a long exposure. +One well-known case of an astrograph used in a discovery is Clyde Tombaugh's discovery of the dwarf planet Pluto in 1930. Tombaugh was given the job of hunting for a suspected "9th planet" to be achieved by systematically photographing the area of the sky around the ecliptic. Tombaugh used Lowell Observatory's 13-inch (330 mm) (3 lens element), f/5.3 refractor astrograph, which recorded images on 14-by-17-inch (360 mm × 430 mm) glass plates. + + +== Use in amateur astrophotography == +In the amateur astronomy field, many types of commercial and amateur built telescopes are designed for astrophotography and labeled "astrographs". Optical designs of amateur astrographs vary widely but include apochromatic refractors, variations of Cassegrain reflectors, and Newtonian reflectors. Most optical designs do not produce large, flat, and well-corrected imaging fields and therefore require some type of optical correction by way of field flatteners or coma correctors. Amateur astrographs typically have purpose-built focusers, are constructed of thermally stable materials like carbon fiber, and are put on heavy duty mounts to facilitate accurate tracking of deep sky objects for long periods of time. + + +== See also == +BOOTES +List of telescope types + + +== References == + + +== External links == +The Double Astrograph of the Yale Southern Observatory +The Carnegie Double Astrograph +Pluto Imaging Challenge: Images +Construction of the Tycho Reference Catalogue – 2 Source Catalogues \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Astrolabe-0.md b/data/en.wikipedia.org/wiki/Astrolabe-0.md index 20833a94c..e3b5b47f0 100644 --- a/data/en.wikipedia.org/wiki/Astrolabe-0.md +++ b/data/en.wikipedia.org/wiki/Astrolabe-0.md @@ -4,7 +4,7 @@ chunk: 1/5 source: "https://en.wikipedia.org/wiki/Astrolabe" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:26.368952+00:00" +date_saved: "2026-05-05T09:40:07.689542+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Astrolabe-1.md b/data/en.wikipedia.org/wiki/Astrolabe-1.md index 73035d972..725b5dc05 100644 --- a/data/en.wikipedia.org/wiki/Astrolabe-1.md +++ b/data/en.wikipedia.org/wiki/Astrolabe-1.md @@ -4,7 +4,7 @@ chunk: 2/5 source: "https://en.wikipedia.org/wiki/Astrolabe" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:26.368952+00:00" +date_saved: "2026-05-05T09:40:07.689542+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Astrolabe-2.md b/data/en.wikipedia.org/wiki/Astrolabe-2.md index bed87ac63..55bd4c2aa 100644 --- a/data/en.wikipedia.org/wiki/Astrolabe-2.md +++ b/data/en.wikipedia.org/wiki/Astrolabe-2.md @@ -4,7 +4,7 @@ chunk: 3/5 source: "https://en.wikipedia.org/wiki/Astrolabe" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:26.368952+00:00" +date_saved: "2026-05-05T09:40:07.689542+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Astrolabe-3.md b/data/en.wikipedia.org/wiki/Astrolabe-3.md index ee74601ed..e1546fff6 100644 --- a/data/en.wikipedia.org/wiki/Astrolabe-3.md +++ b/data/en.wikipedia.org/wiki/Astrolabe-3.md @@ -4,7 +4,7 @@ chunk: 4/5 source: "https://en.wikipedia.org/wiki/Astrolabe" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:26.368952+00:00" +date_saved: "2026-05-05T09:40:07.689542+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Astrolabe-4.md b/data/en.wikipedia.org/wiki/Astrolabe-4.md index 3aab2cc45..06232e30e 100644 --- a/data/en.wikipedia.org/wiki/Astrolabe-4.md +++ b/data/en.wikipedia.org/wiki/Astrolabe-4.md @@ -4,7 +4,7 @@ chunk: 5/5 source: "https://en.wikipedia.org/wiki/Astrolabe" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:26.368952+00:00" +date_saved: "2026-05-05T09:40:07.689542+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Astronomical_clock-0.md b/data/en.wikipedia.org/wiki/Astronomical_clock-0.md index 9d42603f9..2456f0f77 100644 --- a/data/en.wikipedia.org/wiki/Astronomical_clock-0.md +++ b/data/en.wikipedia.org/wiki/Astronomical_clock-0.md @@ -4,7 +4,7 @@ chunk: 1/7 source: "https://en.wikipedia.org/wiki/Astronomical_clock" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:27.581434+00:00" +date_saved: "2026-05-05T09:40:22.228447+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Astronomical_clock-1.md b/data/en.wikipedia.org/wiki/Astronomical_clock-1.md index 2357ad4b0..50cf5f1bd 100644 --- a/data/en.wikipedia.org/wiki/Astronomical_clock-1.md +++ b/data/en.wikipedia.org/wiki/Astronomical_clock-1.md @@ -4,7 +4,7 @@ chunk: 2/7 source: "https://en.wikipedia.org/wiki/Astronomical_clock" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:27.581434+00:00" +date_saved: "2026-05-05T09:40:22.228447+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Astronomical_clock-2.md b/data/en.wikipedia.org/wiki/Astronomical_clock-2.md index ce28455c3..ca1c2633b 100644 --- a/data/en.wikipedia.org/wiki/Astronomical_clock-2.md +++ b/data/en.wikipedia.org/wiki/Astronomical_clock-2.md @@ -4,7 +4,7 @@ chunk: 3/7 source: "https://en.wikipedia.org/wiki/Astronomical_clock" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:27.581434+00:00" +date_saved: "2026-05-05T09:40:22.228447+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Astronomical_clock-3.md b/data/en.wikipedia.org/wiki/Astronomical_clock-3.md index b106d006b..cb3d8f51c 100644 --- a/data/en.wikipedia.org/wiki/Astronomical_clock-3.md +++ b/data/en.wikipedia.org/wiki/Astronomical_clock-3.md @@ -4,7 +4,7 @@ chunk: 4/7 source: "https://en.wikipedia.org/wiki/Astronomical_clock" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:27.581434+00:00" +date_saved: "2026-05-05T09:40:22.228447+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Astronomical_clock-4.md b/data/en.wikipedia.org/wiki/Astronomical_clock-4.md index 3a89981c6..929301c85 100644 --- a/data/en.wikipedia.org/wiki/Astronomical_clock-4.md +++ b/data/en.wikipedia.org/wiki/Astronomical_clock-4.md @@ -4,7 +4,7 @@ chunk: 5/7 source: "https://en.wikipedia.org/wiki/Astronomical_clock" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:27.581434+00:00" +date_saved: "2026-05-05T09:40:22.228447+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Astronomical_clock-5.md b/data/en.wikipedia.org/wiki/Astronomical_clock-5.md index 28d00a4d6..0fb18d2df 100644 --- a/data/en.wikipedia.org/wiki/Astronomical_clock-5.md +++ b/data/en.wikipedia.org/wiki/Astronomical_clock-5.md @@ -4,7 +4,7 @@ chunk: 6/7 source: "https://en.wikipedia.org/wiki/Astronomical_clock" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:27.581434+00:00" +date_saved: "2026-05-05T09:40:22.228447+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Astronomical_clock-6.md b/data/en.wikipedia.org/wiki/Astronomical_clock-6.md index 0936ff56d..9c6aa45f8 100644 --- a/data/en.wikipedia.org/wiki/Astronomical_clock-6.md +++ b/data/en.wikipedia.org/wiki/Astronomical_clock-6.md @@ -4,7 +4,7 @@ chunk: 7/7 source: "https://en.wikipedia.org/wiki/Astronomical_clock" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:27.581434+00:00" +date_saved: "2026-05-05T09:40:22.228447+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Astronomical_rings-0.md b/data/en.wikipedia.org/wiki/Astronomical_rings-0.md index 902991a4f..b32f9c597 100644 --- a/data/en.wikipedia.org/wiki/Astronomical_rings-0.md +++ b/data/en.wikipedia.org/wiki/Astronomical_rings-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Astronomical_rings" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:29.975083+00:00" +date_saved: "2026-05-05T09:40:08.950204+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Autoguider-0.md b/data/en.wikipedia.org/wiki/Autoguider-0.md new file mode 100644 index 000000000..4b4665a35 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Autoguider-0.md @@ -0,0 +1,28 @@ +--- +title: "Autoguider" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Autoguider" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:10.121265+00:00" +instance: "kb-cron" +--- + +An autoguider is an automatic electronic guidance tool used in astronomy to keep a telescope pointed precisely at an object being observed. This prevents the object from drifting across the field of view during long-exposures which would create a blurred or elongated image. + + +== Usage == +Imaging of dim celestial targets, usually deep sky objects, requires exposure times of many minutes, particularly when narrowband images are being taken. In order for the resulting image to maintain usable clarity and sharpness during these exposures, the target must be held at the same position within the telescope's field of view during the whole exposure; any apparent motion would cause point sources of light (such as stars) to appear as streaks, or the object being photographed to appear blurry. Even computer-tracked mounts and GoTo telescopes do not eliminate the need for tracking adjustments for exposures beyond a few minutes, as astrophotography demands an extremely high level of precision that these devices typically cannot achieve, especially if the mount is not properly polar aligned. +To accomplish this automatically an autoguider is usually attached to either a guidescope or finderscope, which is a smaller telescope oriented in the same direction as the main telescope, or an off-axis guider, which uses a prism to divert some of the light originally headed towards the eyepiece. +The device has a CCD or CMOS sensor that regularly takes short exposures of an area of sky near the object. After each image is captured, a computer measures the apparent motion of one or more stars within the imaged area and issues the appropriate corrections to the telescope's computerized mount. +Some computer controlled telescope mounts have an autoguiding port that connects directly to the autoguider (usually referred to as an ST-4 port, which works with analog signals). In this configuration, a guide camera will detect any apparent drift in the field of view. It will then send this signal to a computer which can calculate the required correction. This correction is then sent back to the camera which relays it back to the mount. +An autoguider need not be an independent unit; some high-end CCD imaging units (such as those offered by SBIG) have a second, integrated CCD sensor on the same plane as the main imaging chip that is dedicated to autoguiding. Astronomical video cameras or modified webcams can also serve as an autoguiding unit when used with guiding software such as Guidedog or PHD2, or general-purpose astronomical programs such as MaxDSLR. However, these setups are generally not as sensitive as specialized units. +Since an image of a star can take up more than one pixel on an image sensor due to lens imperfections and other effects, autoguiders use the amount of light falling on each pixel to calculate where the star should actually be located. As a result, most autoguiders have subpixel accuracy. In other words, the star can be tracked to an accuracy better than the angular size represented by one CCD pixel. However, atmospheric effects (astronomical seeing) typically limit accuracy to one arcsecond in most situations. To prevent the telescope from moving in response to changes in the guide star's apparent position caused by seeing, the user can usually adjust a setting called "aggressiveness". + + +== Notes == + + +== References == +Lodriguss, Jerry. "Catching the Light." http://www.astropix.com/HTML/I_ASTROP/TRACKED/AUTOG.HTM +Covington, Michael. Digital SLR Astrophotography. New York: Cambridge University Press, 2007 \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Backstaff-0.md b/data/en.wikipedia.org/wiki/Backstaff-0.md index 18704b374..d83dfeac1 100644 --- a/data/en.wikipedia.org/wiki/Backstaff-0.md +++ b/data/en.wikipedia.org/wiki/Backstaff-0.md @@ -4,7 +4,7 @@ chunk: 1/3 source: "https://en.wikipedia.org/wiki/Backstaff" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:31.201916+00:00" +date_saved: "2026-05-05T09:40:11.293304+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Backstaff-1.md b/data/en.wikipedia.org/wiki/Backstaff-1.md index d9a353319..67ce6f747 100644 --- a/data/en.wikipedia.org/wiki/Backstaff-1.md +++ b/data/en.wikipedia.org/wiki/Backstaff-1.md @@ -4,7 +4,7 @@ chunk: 2/3 source: "https://en.wikipedia.org/wiki/Backstaff" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:31.201916+00:00" +date_saved: "2026-05-05T09:40:11.293304+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Backstaff-2.md b/data/en.wikipedia.org/wiki/Backstaff-2.md index 1a1e9b500..65e960ce9 100644 --- a/data/en.wikipedia.org/wiki/Backstaff-2.md +++ b/data/en.wikipedia.org/wiki/Backstaff-2.md @@ -4,7 +4,7 @@ chunk: 3/3 source: "https://en.wikipedia.org/wiki/Backstaff" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:31.201916+00:00" +date_saved: "2026-05-05T09:40:11.293304+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Barcelona_astrolabe-0.md b/data/en.wikipedia.org/wiki/Barcelona_astrolabe-0.md index 18250195b..b78920018 100644 --- a/data/en.wikipedia.org/wiki/Barcelona_astrolabe-0.md +++ b/data/en.wikipedia.org/wiki/Barcelona_astrolabe-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Barcelona_astrolabe" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:33.541647+00:00" +date_saved: "2026-05-05T09:40:12.559441+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Bris_sextant-0.md b/data/en.wikipedia.org/wiki/Bris_sextant-0.md new file mode 100644 index 000000000..c45be5763 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Bris_sextant-0.md @@ -0,0 +1,33 @@ +--- +title: "Bris sextant" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Bris_sextant" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:13.805334+00:00" +instance: "kb-cron" +--- + +The Bris sextant , or Bris Mini-Sextant, is not a sextant proper, but is a small angle-measuring device that can be used for navigation. The Bris is, however, a true reflecting instrument which derives its high accuracy from the same principle of double reflection which is fundamental to the octant, the true sextant, and other reflecting instruments. It differs from other sextants primarily in being a fixed angle sextant, capable of measuring a few specific angles. + + +== History == +Sven Yrvind (Lundin) developed his Bris sextant in or before 2007 as part of his quest for low-cost, low-technology equipment for ocean crossings. The Bris is a low-technology, high-precision, fixed-interval instrument. It is made of two narrow, flat pieces of glass (microscope slides) permanently and rigidly mounted in a V-shape to a third flat piece of #12 welding glass to make viewing the sun eye safe. When the sun or moon is viewed through the V, it is split into eight images. The instrument is small and rugged enough that it can be kept in a 35mm film canister (water-tigh, about 3 cm diameter, 4 cm tall) on a lanyard around one's neck. +The Bris sextant is calibrated at a known geographic position with a good clock and a nautical almanac. As the day passes, one works the sight reductions backwards to develop exact angles for each of the images' tops and bottoms. The Sun and Moon have approximately the same angular size from the surface of the Earth, and can use the same calibrations. +In use, one waits until an image's edge touches the horizon, and then records the time and reduces the sight using the recorded angle for that edge of the image. + + +== Etymology == +Bris is Swedish for breeze. The name Bris is used by Yrvind for a number of his sail boats. + + +== References == + + +== Sources == +A three-page article (not available online) on the Bris sextant appeared in Yachting Monthly magazine, June 1997. +A two-page article (not available online) on the Bris sextant appeared in Die Yacht magazine, 22/1997: Mini-Sextant: Mit einem genial einfachen Gerät verblufft Weltumsegler Sven Lundin jetzt die gesamte Fachwelt. +Bris Mini Sextant Instructions, page 2, Sven Yrvind, 1998 + + +== External links == \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/CCOR-2-0.md b/data/en.wikipedia.org/wiki/CCOR-2-0.md new file mode 100644 index 000000000..6d45088e0 --- /dev/null +++ b/data/en.wikipedia.org/wiki/CCOR-2-0.md @@ -0,0 +1,195 @@ +--- +title: "CCOR-2" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/CCOR-2" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:15.017695+00:00" +instance: "kb-cron" +--- + +CCOR-2 (Compact CORonograph 2) is the second space coronograph of Compact Coronograph series and the first one in the series CCOR-1 on GOES-19. It is located aboard SOLAR-1 spacecraft (named SWFO-L1 before reaching its destination) placed at Lagrange 1 point – about 1.5 million kilometers (~930,000 miles) from the Earth towards the Sun. It will orbit the Sun at a distance between 0.974 and 1.006 AU. +It was launched in September 2025 from Florida. + + +== Mission == +CCOR-2 will provide low latency, high cadence visible light (the spectrum a human eye sees) images of solar corona and its surroundings. It will observe coronal mass ejections (CME) that are potentially dangerous to electronic infrastructure and because of that its data is going to be used for space weather forecasting. CCOR coronographs are descendants of aging SOHO/LASCO and STEREO/COR instruments. +It was primarily made for National Oceanic and Atmospheric Administration and Space Weather Prediction Center. + + +=== Launch and destination === +It was launched aboard SpaceX Falcon 9 Rocket from Kennedy Space Flight Center located on eastern Florida at 7:30 AM EDT on 24 September 2025. It has reached L1 point on 23 January 2026 – that day its first light image was taken too. + + +==== Forecasting ==== +CCOR data (including CCOR-2) are used for space weather prediction. PyCAT (open source software designed by NOAA/SPWC and UK Met Office) and WSA-Enlil model are fed with coronograph data in order to perform calculations of CME mass, velocity and importantly – direction. + + +== Parameters and technical data == + +CCOR-2 was developed by US Naval Research Laboratory in Washington D.C. It has a length of about 72 centimeters (28.3 in) and due to its small size it's called Compact Coronograph. It features a 2048×1920 pixels Active Pixel Sensor detector which detects wavelengths in the range of ~450 nm to ~750 nm. +The instrument has to follow several requirements, listed below. + +A spatial resolution of ≤70 arcseconds +Inner FOV geometric cutoff at 3.0 solar radii ( + + + + + R + + ⊙ + + + + + {\displaystyle R_{\odot }} + +) +Outer FOV at 20 + + + + + R + + ⊙ + + + + + {\displaystyle R_{\odot }} + +or better +A signal to noise ratio of 10 in the region between 4.4 + + + + + R + + ⊙ + + + + + {\displaystyle R_{\odot }} + + and 22.7 + + + + + R + + ⊙ + + + + + {\displaystyle R_{\odot }} + + (1.17° to 6.05°) +Maximum image latency of 30 minutes +CME mass estimate with an error of ≤50 per cent for CMEs with mass between + + + + 1.0 + × + + 10 + + 7 + + + + + {\displaystyle 1.0\times 10^{7}} + +kg and + + + + 5.0 + × + + 10 + + 14 + + + + + {\displaystyle 5.0\times 10^{14}} + +kg +A closable outer door +Full resolution image cadence of 15 minutes or 5 minutes for 2x2 binned images. +Minimum signal intensity above noise of + + + + ≥ + 1.0 + × + + 10 + + − + 11 + + + + + {\displaystyle \geq 1.0\times 10^{-11}} + + + + + + + B + + ⊙ + + + + + {\displaystyle B_{\odot }} + + ( + + + + + B + + ⊙ + + + + + {\displaystyle B_{\odot }} + + is solar surface brightness – about -10.8 mag/arcsec²) +Coronal brightness measurement with error up to 10% +CME velocity estimate with biggest allowed error of 5% in the range of 200 km/s to 3400 km/s +At least five years of operations with resources enough for additional five years (requirement for entire spacecraft) +CCOR-2 shall be able to meet all the requirements when observing during an X50 solar flare or S4 class solar storm +Observing in visible light +The data must be available for SWPC reach within 30 minutes of its creation +CCOR shall be capable of surviving 5 years on orbit before start of operations + + +==== Actual specifications ==== + + +=== Ground Processing Algorithm === +CCOR-2 images are available in FITS format, however they are also processed on the ground. +The first level of the images is L0 CCSDS which is a raw readout of detector pixels. L0 CCSDS is then rotated so solar north points upwards which creates a L0B file. +Level 1A image is formed by converting DN value of pixel into Mean Solar Brightness unit, division by exposure time, correcting for vignetting and detector linearity rectification. It is the main operational product used for forecasting. +A median background is created from L1 by computing F-corona and stray-light based of the image. L1A with background subtraction, distortion correction application and flat field rectification creates L2 image. + + +== References == \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Celatone-0.md b/data/en.wikipedia.org/wiki/Celatone-0.md new file mode 100644 index 000000000..08e0c9006 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Celatone-0.md @@ -0,0 +1,31 @@ +--- +title: "Celatone" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Celatone" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:16.196142+00:00" +instance: "kb-cron" +--- + +The celatone was a device invented by Galileo Galilei to observe Jupiter's moons with the purpose of finding longitude on Earth. It took the form of a piece of headgear with a telescope taking the place of an eyehole. + + +== Modern versions == +In 2013, Matthew Dockrey created a replica celatone, using notes from a version created by Samuel Parlour. From April 2014 to January 2015, Dockrey's celatone was on display in the Royal Observatory, Greenwich in east London. + + +== See also == +Longitude prize +Galilean moons + + +== References == + +Sobel, Dava (1995). Longitude: The True Story of a Lone Genius Who Solved the Greatest Scientific Problem of His Time. Penguin. ISBN 0-14-025879-5. + + +== External links == +Video animation of a Celatone and its use in discovering the longitude for marine navigation +Dockrey celatone +"Apparatus to render a telescope manageable on shipboard" \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Celestial_Sphere_Woodrow_Wilson_Memorial-0.md b/data/en.wikipedia.org/wiki/Celestial_Sphere_Woodrow_Wilson_Memorial-0.md index a4db2ce15..1b6bd23ea 100644 --- a/data/en.wikipedia.org/wiki/Celestial_Sphere_Woodrow_Wilson_Memorial-0.md +++ b/data/en.wikipedia.org/wiki/Celestial_Sphere_Woodrow_Wilson_Memorial-0.md @@ -4,7 +4,7 @@ chunk: 1/2 source: "https://en.wikipedia.org/wiki/Celestial_Sphere_Woodrow_Wilson_Memorial" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:38.333218+00:00" +date_saved: "2026-05-05T09:40:17.455936+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Celestial_Sphere_Woodrow_Wilson_Memorial-1.md b/data/en.wikipedia.org/wiki/Celestial_Sphere_Woodrow_Wilson_Memorial-1.md index 2432c9a53..61c80957e 100644 --- a/data/en.wikipedia.org/wiki/Celestial_Sphere_Woodrow_Wilson_Memorial-1.md +++ b/data/en.wikipedia.org/wiki/Celestial_Sphere_Woodrow_Wilson_Memorial-1.md @@ -4,7 +4,7 @@ chunk: 2/2 source: "https://en.wikipedia.org/wiki/Celestial_Sphere_Woodrow_Wilson_Memorial" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:38.333218+00:00" +date_saved: "2026-05-05T09:40:17.455936+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Center_for_Detectors-0.md b/data/en.wikipedia.org/wiki/Center_for_Detectors-0.md new file mode 100644 index 000000000..fc9f245fe --- /dev/null +++ b/data/en.wikipedia.org/wiki/Center_for_Detectors-0.md @@ -0,0 +1,58 @@ +--- +title: "Center for Detectors" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Center_for_Detectors" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:18.644024+00:00" +instance: "kb-cron" +--- + +The Center for Detectors (CfD) is a Rochester Institute of Technology College of Science academic research center. The CfD, established in January 2010 by Dr. Donald Figer, began as an expansion of the Rochester Imaging Detector Laboratory. Its mission is to enable scientific discovery, national security, better living, and commercial innovation through the design and development of advanced photon detectors and associated technology. +The CfD designs, develops, and implements new advanced sensor technologies through collaboration with academic researchers, industry engineers, government scientists, and university students. The mission of the CfD is to enable scientific discovery, national security, better living, and commercial innovation through the design and development of advanced photon detectors and associated technology in a broad array of applications (e.g. astrophysics, biomedical imaging, Earth system science, and inter-planetary travel). + + +== Research == + +The CfD uses a multi-disciplinary approach, spanning the many branches of engineering, imaging science, physics and astronomy. Research pillars of the CfD include, Detectors and Instrumentation, Observational Astrophysics, Wideband Gap Materials, Nanostructures, and Silicon Photonics. + + +=== Detectors and Instrumentation === +A primary objective of the CfD is the development of advanced detectors and instrumentation for cross-disciplinary applications. Major research projects include the development of detectors that can sense individual photons, cover very large areas of the sky, and have excellent sensitivity in ultraviolet and infrared wavelengths. These devices have specifications that make them ideal for the next generation of large ground-based and space-based astronomical telescopes, for applications such as finding another Earth and determining the nature of dark energy and dark matter. The CfD is also developing two dimensional arrays of micromirrors for astronomical applications. + + +=== Observational astrophysics === +This area includes observational research programs spanning the nearby universe of stars and the interstellar medium within the Galaxy to cosmological observations of the large-scale structure of the universe, including studies of fundamental physics. Projects include works that aim to elucidate the nature of the cosmos on the largest scales and most distant times. Other programs include the identification of the upper mass limit to stars and the search for young massive star clusters in the Galaxy. It also includes leadership roles on major future astronomy telescope panels to specify the detector requirements needed in order to satisfy mission science requirements. + + +=== Wideband gap materials === +The Semiconductor Photonics and Electronics Group develops III-V and III-Nitride semiconductors for photonic, optoelectronic, and electronic devices as promising candidates for next generation communication and illumination systems. + + +=== Nanostructures === +The Epitaxially-Integrated Nanoscale Systems Laboratory in the CfD develops nanostructures using epitaxy of III-V semiconductors on 2-D nanosheets. The research focuses on the growth of various nanostructures, including nanowires and nanofins, by metal-organic chemical vapor deposition through a synthesis process known as selective chemical etching for room temperature benchtop fabrication of flexible III-V nanostructure based optoelectronic and photovoltaic devices. + + +=== Silicon photonics === +The CfD Integrated Photonics Group develops photonic technology for broad application in commercial, defense, and scientific applications. It also leads a program for integrated photonics education. This area of research is focused on novel silicon photonic devices with the goal of realizing high performance computing communication, and sensing systems that leverage high speed, bandwidth, and sensitivity to light. +The Center for Detectors benefits from employees that come from a diverse range of academic programs and professional occupations. The CfD staff includes professors, engineers, and students (undergraduate, masters, and PhD). +CfD is grant-funded and has been awarded more than $40M in external funding since 2006. Primary sponsors include NASA, National Science Foundation, and the Gordon and Betty Moore Foundation. Additional sources of funding include Thermo Fisher Scientific, NASA Jet Propulsion Laboratory, ITT Excelis, and Smithsonian Astrophysical Observatory. + + +== Outreach and Communications == +Undergraduate researchers at the RIT Center for Detectors come from over a dozen different majors and “check their major at the door” because they will become expert in a new type of major in the CfD – the major of “solving real-world research problems.” Authentic research experiences at the Center for Detectors put students clearly in the critical path of externally funded projects, a high risk/high reward gambit that has proven to burnish the capabilities of CfD students who have gone out in the world and made outsized impact, such as at Ball Aerospace and SpaceX. Students work in multidisciplinary teams to apply what they know, teach each other and seek out resources necessary for advancing their project. Another key feature in undergraduate research experiences at the center—and what makes them “real”—is the fact that the students are not doing the research to earn a grade or a certain number of credit hours. The “CfD-experience” trains students to navigate research problems with creativity and resourcefulness. +CfD team members have been published in many journals and publications. CfD members were published in over 35 papers in journals such as The Astrophysical Journal and Optics Express in 2018. CfD research was highlighted in popular publications such as the Scientific American and Forbes online. In 2018, CfD members served as expert commentators in articles Astronomy magazine and New Scientist and as expert authors of strategic planning documents for NASA. For a complete list of CfD member publications go here: CfD Publications. + + +== Equipment and facilities == + +The Center for Detectors (CfD) is located in Engineering Hall (Building 17) at the Rochester Institute of Technology. The CfD headquarters consists of 7,000 square feet of office and research laboratory space. The lab space includes the Rochester Imaging Detector Laboratory, the Lobozzo Photonics and Optical Characterization Laboratory, the Integrated Photonics Laboratory, the Laboratory for Experimental Cosmology, the Laboratory for Advanced Instrumentation Research (LAIR), the Quantum Imaging and Information Laboratory, and the Electrical and Optical Characterization Lab for LED devices. + + Facilities within CfD include a permanent clean room, ESD stations, vacuum pumping systems, liquid and closed-cycle cryogenic dewars, optical benches, flow tables, light sources, UV-IR monochromators, thermal control systems, cryogenic motion control systems, single-photon detector systems, a cryogenic optoelectronic probe station, vibration testing stations, a suborbital rocket payload assembly area, power supplies, general lab electronics, and data reduction computers. In addition to these dedicated facilities, the CfD has access to facilities within the Semiconductor and Microsystems Fabrication Laboratory (SMFL) and other areas across the RIT campus. + + +== References == + + +== External links == +Projects \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Cherenkov_Telescope_Array_Observatory-0.md b/data/en.wikipedia.org/wiki/Cherenkov_Telescope_Array_Observatory-0.md new file mode 100644 index 000000000..a1098f4b4 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Cherenkov_Telescope_Array_Observatory-0.md @@ -0,0 +1,48 @@ +--- +title: "Cherenkov Telescope Array Observatory" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Cherenkov_Telescope_Array_Observatory" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:19.807251+00:00" +instance: "kb-cron" +--- + +The Cherenkov Telescope Array Observatory (CTAO) is a multinational project to build a new generation of ground-based gamma-ray instruments in the energy range extending from some tens of GeV to about 300 TeV. It is proposed as an open observatory and will consist of two arrays of imaging atmospheric Cherenkov telescopes, a first array in the Northern Hemisphere, on the Spanish island of La Palma, with emphasis on the study of extragalactic objects at the lowest possible energies, and a second array in the Southern Hemisphere, in the Atacama Desert in Chile, which is to cover the full energy range and concentrate on galactic sources. The physics program of the CTAO goes beyond high-energy astrophysics into cosmology and fundamental physics. +Building on the technology of current-generation ground-based gamma-ray detectors (MAGIC, HESS, and VERITAS), the CTAO will be ten times more sensitive and have unprecedented accuracy in its detection of high-energy gamma rays. Current gamma-ray telescope arrays host up to five individual telescopes, but the CTAO is designed to detect gamma rays over a larger area and a wider range of views, with more than 60 telescopes located in the northern and southern hemispheres. +In January 2025, the CTAO was established as a European Research Infrastructure Consortium (ERIC) by the European Commission. +The project is part of the Aspera European Astroparticle network and of Astronet. + + +== Locations == + +The CTAO headquarters is hosted by Italy's National Institute for Astrophysics, and the Science Data Management Centre is hosted by the Deutsches Elektronen-Synchrotron in Zeuthen, Germany. +The CTAO's northern-hemisphere site, CTAO-North, is located on the existing site of the  Instituto de Astrofísica de Canarias' Roque de los Muchachos Observatory, on the island of La Palma, the fifth largest of the Canary Islands. At 2,200 metres of altitude and nestled on a plateau below the rim of an extinct volcanic crater, the site hosts a prototype of the LST, the LST-1, and LST-2, LST-3, and LST-4 are under construction. The site will also host MSTs. +The CTAO's southern-hemisphere site, CTAO-South, is located less than 10 km southeast of the ESO's Paranal Observatory, in the Atacama Desert of Chile. The site will host MSTs and SSTs. + + +== Science == + +The CTAO will look at higher-energy photons than ever measured before. Its cosmic particle accelerators can reach energies inaccessible to such accelerators as the Large Hadron Collider. The CTAO will seek to understand the impact of high-energy particles in the evolution of cosmic systems and to gain insight into the most extreme and unusual phenomena in the Universe. It will also search for annihilating dark matter particles and deviations from Einstein's theory of special relativity, even conducting a census of particle acceleration in the universe. +Research at the CTAO will seek to address questions in and beyond astrophysics. The CTAO's observations will include the following key targets: Galactic Center, Large Magellanic Cloud, Galactic Plane, galaxy clusters, cosmic ray PeVatrons, star-forming systems, active galactic nuclei, and transient phenomena. + + +== Possible increase of light pollution == +There was a planned INNA megaproject by AES Andes, which would have installed 1,000 light sources just five km from the southern part of the CTAO, which had threatened to increase light pollution at the location by 55%. However, it was announced to have been cancelled on 23 January 2026. + + +== See also == +Cherenkov radiation +List of telescope types +Major Atmospheric Cerenkov Experiment Telescope +Pavel Cherenkov +Segmented mirror + + +== References == + + +== External links == + +Official website +European Commission's Decision to Establish the CTAO as an ERIC \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Chronocinematograph-0.md b/data/en.wikipedia.org/wiki/Chronocinematograph-0.md new file mode 100644 index 000000000..d8cda46e0 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Chronocinematograph-0.md @@ -0,0 +1,15 @@ +--- +title: "Chronocinematograph" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Chronocinematograph" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:20.990137+00:00" +instance: "kb-cron" +--- + +Chronocinematograph is an astronomical instrument consisting of a film camera, chronometer and chronograph. The device records images using a more precise timetable for observing an eclipse. It was invented in 1927 by a Polish astronomer, mathematician and geodesist Tadeusz Banachiewicz for observing total solar eclipses. During the same year, Banachiewcz used his device for solar observations in Lapland (Sweden), then in the US (1932) and Greece, Japan and Siberia (1936). +The invention enhanced the precision for determining the time of an eclipse, due to more precisely timed photos of Baily's beads, and quantifying the duration of totality. This could not have been observed as closely as before due to the brightness of the sun. + + +== References == \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Cosmolabe-0.md b/data/en.wikipedia.org/wiki/Cosmolabe-0.md new file mode 100644 index 000000000..1a5ac8d1f --- /dev/null +++ b/data/en.wikipedia.org/wiki/Cosmolabe-0.md @@ -0,0 +1,26 @@ +--- +title: "Cosmolabe" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Cosmolabe" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:24.500974+00:00" +instance: "kb-cron" +--- + +The cosmolabe was an ancient astronomical instrument resembling the astrolabe, formerly used for measuring the angles between heavenly bodies. It is also called pantacosm. Jacques Besson also uses this name, or universal instrument, for his invention described in Le cosmolabe (1566), which could be used for astrometry, cartography, navigation, and surveying. +The Cosmolabe is a comprehensive and versatile astronomical instrument designed to perform a wide range of observations and calculations. It was created to serve as a universal tool, capable of replacing several different instruments used in astronomy, geometry, and navigation. According to the inventor, the Cosmolabe can perform the functions of the Sphere, various types of Astrolabes (including the Armillary of Ptolemy, the Torquetum, and the Triquetrum), Jacob’s staff, the Geometric Square, the astronomical quadrant, and even celestial and terrestrial globes. +The instrument is designed to be leveled precisely with the horizon, and it can be used on any flat plane, regardless of its inclination. With the Cosmolabe, users can easily determine the meridian line, find the vertical and horizontal circles (almucantarats and height circles), and represent all circles of declination on a given horizon. Additionally, the Cosmolabe can be used to mark meridional circles and find the great circle passing through any two points in the sky. +A key feature of the Cosmolabe is its ability to determine the longitudes of places on Earth, both for land and sea navigation. It allows for the calculation of time and the creation of sundials on any plane. Furthermore, the instrument can be used to measure the height of the Pole using a notable northern star, determine the degree of the Sun for a given day, and find the length of the day at any location. +The Cosmolabe is also designed for practical applications in navigation, allowing for the measurement of distances between locations, the creation of chorographic maps and geographic globes, and the calculation of the route and longitude of places for maritime navigation. Its versatility extends to finding the longitudes of places by observing celestial bodies such as comets, the Moon, and fixed stars. +In summary, the Cosmolabe offers a vast array of astronomical, geographical, and navigational functions, making it an essential instrument for scientists, navigators, and mathematicians. Its simplicity and universal application were praised by its inventor, who argued that it could replace multiple other instruments and provide a more efficient and precise means of conducting observations and calculations. + + +== Notes == + + +== References == +"'Le Cosmolabe Ou Instrument Universel : Concernant Toutes Observations qui se peuvent faire Par les Sciences Mathematiques, Tant au Ciel, en la Terre, comme en la Mer' - Viewer | MDZ". + This article incorporates text from this source, which is in the public domain. Porter, Noah, ed. (1913). Webster's Dictionary. Springfield, Massachusetts: C. & G. Merriam Co. {{cite encyclopedia}}: Missing or empty |title= (help) + This article incorporates text from a publication now in the public domain: Chambers, Ephraim, ed. (1728). Cyclopædia, or an Universal Dictionary of Arts and Sciences (1st ed.). James and John Knapton, et al. {{cite encyclopedia}}: Missing or empty |title= (help) +This book, written in the old french language, is the original book "Le Cosmolabe", September 1566, by Professor of Sciences in Orlean, Jacques Besson, Paris/France and is in the public domain. \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Cranmer_Park-0.md b/data/en.wikipedia.org/wiki/Cranmer_Park-0.md new file mode 100644 index 000000000..0d246b5fa --- /dev/null +++ b/data/en.wikipedia.org/wiki/Cranmer_Park-0.md @@ -0,0 +1,25 @@ +--- +title: "Cranmer Park" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Cranmer_Park" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:25.682353+00:00" +instance: "kb-cron" +--- + +Cranmer Park is a city park in Denver, United States located in the Hilltop neighborhood off Colorado Boulevard between East 1st and East 3rd Avenue. It is notable for its large sundial. +An inscription at the base describes the axis of the gnomon as elevated 39°43' in the direction of polar north. The stone is perpendicular to the gnomon at 50°17', which makes it parallel to the equator. The south side of the stone is similarly marked for wintertime observation. +A polar chart at the base of the sundial describes the zodiac and degrees of the sun's position, and how to set a clock based on the gnomon's shadow. For winter viewing, the chart continues on the south side of the stone. + + +== History of the sundial == +The current sundial is the second one to exist at this location in the park. The first was donated in 1941 by longtime Manager of Denver Parks George E. Cranmer, for whom the park is named. It was destroyed by vandals who exploded dynamite under it in September 1965. The replacement sundial was installed in March, 1966 after a successful citywide fundraising effort led by the Denver Junior Chamber of Commerce. It was restored again in 2018 to repair cracking stones. +The park is on the National Register of Historic Places. + + +== References == + + +== External links == +Save Our Sundial \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument-0.md b/data/en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument-0.md new file mode 100644 index 000000000..93b748aac --- /dev/null +++ b/data/en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument-0.md @@ -0,0 +1,21 @@ +--- +title: "Dark Energy Spectroscopic Instrument" +chunk: 1/3 +source: "https://en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:27.985101+00:00" +instance: "kb-cron" +--- + +The Dark Energy Spectroscopic Instrument (DESI) is a scientific research instrument for conducting spectrographic astronomical surveys of distant galaxies. Its main components are a focal plane containing 5,000 fiber-positioning robots, and a bank of spectrographs which are fed by the fibers. The instrument enables an experiment to probe the expansion history of the universe and the mysterious physics of dark energy. The main DESI survey started in May 2021. DESI sits at an elevation of 6,880 feet (2,100 m), where it has been retrofitted onto the Mayall Telescope on top of Kitt Peak in the Sonoran Desert, which is located 55 miles (89 km) from Tucson, Arizona, United States. +The instrument is operated by the Lawrence Berkeley National Laboratory under funding from the U.S. Department of Energy's Office of Science. Construction of the instrument was principally funded by the U.S. Department of Energy's Office of Science, and by other numerous sources including the U.S. National Science Foundation, the British Science and Technology Facilities Council, France's Alternative Energies and Atomic Energy Commission, Mexico's National Council of Science and Technology, Spain's Ministry of Science and Innovation, by the Gordon and Betty Moore Foundation, by the Heising-Simons Foundation, and by collaborating institutions worldwide. + +== Scientific goals == + +The expansion history and large-scale structure of the universe is a key prediction of cosmological models, and DESI observations will permit scientists to probe various aspects of cosmology, including dark energy, alternatives to general relativity, neutrino masses, and the primordial universe. The data from DESI will be used to create three-dimensional maps of the distribution of matter covering an unprecedented volume of the universe with unparalleled detail. This will provide insight into the nature of dark energy and establish whether cosmic acceleration is due to a cosmic-scale modification of General Relativity. DESI will be transformative in the understanding of dark energy and the expansion rate of the universe at early times, one of the greatest mysteries in the understanding of the physical laws. +DESI will measure the expansion history of the universe using the baryon acoustic oscillations (BAO) imprinted in the clustering of galaxies, quasars, and the intergalactic medium. The BAO technique is a robust way to extract cosmological distance information from the clustering of matter and galaxies. It relies only on very large-scale structure and it does so in a manner that enables scientists to separate the acoustic peak of the BAO signature from uncertainties in most systematic errors in the data. BAO was identified in the 2006 Dark Energy Task Force report as one of the key methods for studying dark energy. In May 2014, the High-Energy Physics Advisory Panel, a federal advisory committee, commissioned by the US Department of Energy (DOE) and the National Science Foundation (NSF) endorsed DESI. + +== 3D map of the universe == + +The baryon acoustic oscillations method requires a three-dimensional map of distant galaxies and quasars created from the angular and redshift information of a large statistical sample of cosmologically distant objects. By obtaining spectra of distant galaxies it is possible to determine their distance, via the measurement of their spectroscopic redshift, and thus create a 3-D map of the universe. The 3-D map of the large-scale structure of the universe also contains more information about dark energy than just the BAO and is sensitive to the mass of the neutrino and parameters that governed the primordial universe. During its five-year survey, which began on May 15, 2021, the DESI experiment is expected to observe 40 million galaxies and quasars. \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument-1.md b/data/en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument-1.md new file mode 100644 index 000000000..b0c1916e6 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument-1.md @@ -0,0 +1,24 @@ +--- +title: "Dark Energy Spectroscopic Instrument" +chunk: 2/3 +source: "https://en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:27.985101+00:00" +instance: "kb-cron" +--- + +== Development == +The DESI instrument implements a new highly multiplexed optical spectrograph on the Mayall Telescope. The new optical corrector design creates a very large, 8.0 square degree field of view on the sky, which combined with the new focal plane instrumentation weighs approximately 10 tonnes. The focal plane accommodates 5,000 small robotic fiber positioners on a 10.4 millimeter pitch. The entire focal plane can be reconfigured for the next exposure in less than two minutes while the telescope slews to the next field. The DESI instrument is capable of taking 5,000 simultaneous spectra over a wavelength range from 360 nm to 980 nm. The DESI project scope included construction, installation, and commissioning of the new wide-field corrector and corrector support structure for the telescope, the focal plane assembly with 5,000 robotic fiber positioners and ten guide/focus/alignment sensors, a 40-meter optical fiber cabling system that brings light from the focal plane to the spectrographs, ten 3-arm spectrographs, an instrument control system, and a data analysis pipeline. +The instrument fabrication was managed by the Lawrence Berkeley National Laboratory and oversees operation of the experiment including a 600-person international scientific collaboration. Cost of construction was $56M from the US Department of Energy's Office of Science plus an additional $19M from other non-federal sources including contributions in-kind. The leadership of DESI currently consists of the director, Dr. Michael E. Levi, collaboration co-spokespersons Prof. Alexie Leauthaud and Prof. Will Percival, project scientists Dr. David J. Schlegel and Dr. Julien Guy, project manager Dr. Patrick Jelinsky, instrument scientists Prof. Klaus Honscheid and Prof. Constance Rockosi. Past collaboration spokespersons have been Prof. Daniel Eisenstein, Prof. Risa Wechsler, Prof. Kyle Dawson, and Dr. Nathalie Palanque-Delabrouille. +The U.S. Department of Energy (DOE) approved CD-0 (Mission Need) on September 18, 2012, approved CD-1 (Alternative Selection and Cost Range) on March 19, 2015, and CD-2 (Performance Baseline) on September 17, 2015. U.S. Congressional approval for the start of DESI as a new Major Item of Equipment was provided in the Fiscal Year 2015 Energy & Water appropriations legislation. Construction on the new instrument started June 22, 2016 with CD-3 (Start Construction) approval and was largely assembled by 2019 with commissioning finishing in March 21, 2020 in advance of the pandemic and marking the formal end of the project (CD-4). DESI was completed under budget by $1.9M and 17 months ahead of schedule. As a consequence, the project received the DOE Project Management Excellence Award for 2020. After a pause for the pandemic and a transition to remote operations, DESI returned to survey operations in December, 2020 with a final checkout and validation phase prior to starting its planned five-year survey. The five-year survey began on May 14, 2021. DESI was shut down for three months in the summer of 2022 due to the Contreras fire which engulfed Kitt Peak. DESI was undamaged and is acquiring scientific data. + +== DESI Legacy Imaging Surveys == +To provide targets for the DESI survey three telescopes surveyed the northern and part of the southern sky in the g, r and z-band. Those surveys were the Beijing-Arizona Sky Survey (BASS), using the Bok 2.3-m telescope, the Dark Energy Camera Legacy Survey (DECaLS), using the Blanco 4m telescope and the Mayall z-band Legacy Survey (MzLS), using the 4-meter Mayall telescope. The area of the surveys is 14,000 square degrees (about one third of the sky) and avoids the Milky Way. These surveys were combined into the DESI Legacy Imaging Surveys, or Legacy Surveys. Colored images of the survey can be viewed in the Legacy Survey Sky Browser. The legacy survey covers 16,000 square degrees of the night sky containing 1.6 billion objects including galaxies and quasars out to 11 billion years ago. + +== History == +DESI received a go-ahead to start R&D for the project in December 2012 with the assignment of the Lawrence Berkeley National Laboratory as the managing laboratory. Dr. Michael Levi, a senior scientist at the Lawrence Berkeley National Laboratory was appointed by the laboratory to be DESI's project director who served in that role starting in 2012 and throughout construction. Henry Heetderks was project manager from 2013 until 2016, Robert Besuner was project manager from 2016 until 2020. Congressional authorization was provided in 2015, and the US Department of Energy's Office of Science approved the start of physical construction in June 2016. First light of the new corrector system was obtained on the night of April 1, 2019, and first-light of the entire instrument was achieved on the night of October 22, 2019. Commissioning ensued after first light and was completed in March 2020, then paused during the pandemic in 2020. DESI started its 5-year main scientific survey on May 14, 2021. DESI is currently operating normally after surviving the Contreras fire in 2022. + +== Data releases == + +All of the publicly available data including redshift catalogs, added-value catalogs, and documentation, can be accessed through DESI data portal. Individuals with accounts at the National Energy Research Scientific Computing Center (NERSC) can access the entire public portion of the DESI data. DESI catalogs also exist in a database format. For convenience, a copy of the public databases is also hosted by the NOIRLab Astro Data Lab science platform, and by using the SPectral Analysis and Retrievable Catalog Lab (SPARCL). One easy way to access DESI spectra online is to use the legacy viewer at the DESI Legacy Imaging Surveys. Users have to check the box for DESI spectra and click on an encircled galaxy or star for a link to the DESI Spectral Viewer to show up. The spectrum can be explored in the DESI Spectral Viewer (see External Links under Index| Legacy Surveys). \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument-2.md b/data/en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument-2.md new file mode 100644 index 000000000..2910f3628 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument-2.md @@ -0,0 +1,36 @@ +--- +title: "Dark Energy Spectroscopic Instrument" +chunk: 3/3 +source: "https://en.wikipedia.org/wiki/Dark_Energy_Spectroscopic_Instrument" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:27.985101+00:00" +instance: "kb-cron" +--- + +=== Early data release === +On 13 June 2023 the DESI Early Data Release (EDR) was announced. The EDR contains spectra of nearly two million galaxies, quasars and stars. One early result of the EDR was announced in February 2023 and described a mass migration of stars into the Andromeda Galaxy. The EDR also revealed very distant quasars and very metal-poor stars. In 2025, a team led by Ragadeepika Pucha of the University of Arizona and the University of Utah reported in The Astrophysical Journal the discovery of the largest number of dwarf galaxies including 2,800 black holes (300 intermediate-mass black holes and 2,500 active black holes) from the EDR. + +==== Possibly evolving dark energy levels ==== +From the level of detail able to be observed, the largest 3-D map of the universe at this point has been created (2024). From this precise data, DESI Director Michael Levi stated:We’re also seeing some potentially interesting differences that could indicate that dark energy is evolving over time. Those may or may not go away with more data, so we’re excited to start analyzing our three-year dataset soon. + +=== Data Release 1 (DR1) === +Data Release 1 (DR1), published on 19 March 2025, contains 18.7 million objects. These objects comprise roughly 4 million stars, 13.1 million galaxies, and 1.6 million quasars. One outcome of these big data were hints of an evolving dark energy. If the data hold, this would mark the first major change in our understanding of the universe in decades. Whilst the DESI observations as such are consistent with the Lambda CDM model, in combination with past surveys of the cosmic microwave background, supernovae, and weak lensing the data show that the influence of dark energy weakens over time. The signal does not reach 5 sigma, but nonetheless at 2.8 to 4.2 sigma heralds a new era of research. The causes of the variation itself are not yet known. + +== See also == +Dark Energy Survey (DES) + +== References == + +== External links == + +Official DESI site +Astronomers complete largest 3D map of the universe ever made. Progress report, Science News, 15 Apr 2026. +Index| Legacy Survey +Legacy Survey Sky Browser +Science Final Design Report +Instrument Final Design Report +DESI data +Key publications +Omnibus DESI collaboration +Telescope tracks 35 million galaxies in Dark Energy hunt, BBC Science report, 28 October 2019 \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Dioptra-0.md b/data/en.wikipedia.org/wiki/Dioptra-0.md index 4bfd8e171..b43ecf743 100644 --- a/data/en.wikipedia.org/wiki/Dioptra-0.md +++ b/data/en.wikipedia.org/wiki/Dioptra-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Dioptra" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:48.449658+00:00" +date_saved: "2026-05-05T09:40:31.436883+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Dividing_engine-0.md b/data/en.wikipedia.org/wiki/Dividing_engine-0.md index 065126f92..f9d808569 100644 --- a/data/en.wikipedia.org/wiki/Dividing_engine-0.md +++ b/data/en.wikipedia.org/wiki/Dividing_engine-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Dividing_engine" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:49.621289+00:00" +date_saved: "2026-05-05T09:40:33.856511+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/ELODIE_spectrograph-0.md b/data/en.wikipedia.org/wiki/ELODIE_spectrograph-0.md new file mode 100644 index 000000000..a9176b3d9 --- /dev/null +++ b/data/en.wikipedia.org/wiki/ELODIE_spectrograph-0.md @@ -0,0 +1,34 @@ +--- +title: "ELODIE spectrograph" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/ELODIE_spectrograph" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:36.183915+00:00" +instance: "kb-cron" +--- + +ELODIE was an echelle spectrograph installed on the 1.93m reflector at the Observatoire de Haute-Provence in south-eastern France. Its optical instrumentation was developed by André Baranne from the Marseille Observatory. The purpose of the instrument was extrasolar planet detection by the radial velocity method. +ELODIE's first light was achieved in 1993. The instrument was decommissioned in August 2006 and replaced in September 2006 by SOPHIE, a new instrument of the same type but with improved features. + + +== Characteristics == +The instrument could observe the electromagnetic spectrum over a wavelength range of 389.5 nm to 681.5 nm in a single exposure, split into 67 spectral orders. The instrument, which was located in a temperature-controlled room, was fed with optical fibers from the Cassegrain focus. The observatory provided an integrated data reduction pipeline which fully reduced the spectra immediately after acquisition and allowed the user to measure radial velocities to an accuracy as good as ±7 m/s. +Over 34,000 spectra were taken with ELODIE, over 20,000 of which are publicly available through a dedicated on-line archive. The instrument was the result of a collaboration between the observatories of Haute-Provence, Geneva and Marseille. A publication describing the instrument appeared in Astronomy & Astrophysics Supplements. + + +== Discovered planets == +The first extrasolar planet to be discovered orbiting a Sun-like star, 51 Pegasi b, was discovered in 1995 using ELODIE. Michel Mayor and Didier Queloz received the Nobel Prize in Physics in 2019 for their achievement. Over twenty such planets have been found with ELODIE. +The instrument was also used to find a planet by the transit method. + + +== See also == +CORALIE spectrograph is a similar instrument at La Silla Observatory in Chile +List of extrasolar planets + + +== References == + + +== External links == +(in English) The ELODIE Archive \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/ESPRESSO-0.md b/data/en.wikipedia.org/wiki/ESPRESSO-0.md new file mode 100644 index 000000000..280253192 --- /dev/null +++ b/data/en.wikipedia.org/wiki/ESPRESSO-0.md @@ -0,0 +1,27 @@ +--- +title: "ESPRESSO" +chunk: 1/2 +source: "https://en.wikipedia.org/wiki/ESPRESSO" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:41.044146+00:00" +instance: "kb-cron" +--- + +ESPRESSO (Echelle Spectrograph for Rocky Exoplanet- and Stable Spectroscopic Observations) is a third-generation, fiber-fed, cross-dispersed, echelle spectrograph mounted on the European Southern Observatory's Very Large Telescope (VLT). The unit saw its first light with one VLT in December 2017 and first light with all four VLT units in February 2018. +ESPRESSO is the successor of a line of echelle spectrometers that include CORAVEL, Elodie, Coralie, and HARPS. It measures changes in the light spectrum with great sensitivity, and is being used to search for Earth-size rocky exoplanets via the radial velocity method. For example, Earth induces a radial-velocity variation of 9 cm/s on the Sun; this gravitational "wobble" causes minute variations in the color of sunlight, invisible to the human eye but detectable by the instrument. The telescope light is fed to the instrument, located in the VLT Combined-Coude Laboratory 70 meters away from the telescope, where the light from up to four unit telescopes of the VLT can be combined. + +== Sensitivity == + +ESPRESSO builds on the foundations laid by the High Accuracy Radial Velocity Planet Searcher (HARPS) instrument at the 3.6-metre telescope at ESO's La Silla Observatory. ESPRESSO benefits not only from the much larger combined light-collecting capacity of the four 8.2-metre VLT Unit Telescopes, but also from improvements in the stability and calibration accuracy that are now possible by laser frequency comb technology. The requirement is to reach 10 cm/s, but the aimed goal is to obtain a precision level of a few cm/s. This would mean a large step forward over current radial-velocity spectrographs such as ESO's HARPS. The HARPS instrument can attain a precision of 97 cm/s (3.5 km/h), with an effective precision of the order of 30 cm/s. The ESPRESSO would greatly exceed this capability making detection of Earth-size planets from ground-based instruments possible. Commissioning of ESPRESSO at the VLT started late 2017. +The instrument is capable of operating in 1-UT mode (using one of the telescopes) and in 4-UT mode. In 4-UT mode, in which all the four 8-m telescopes are connected incoherently to form a 16-m equivalent telescope, the spectrograph detects extremely faint objects. +For example, for G2V type stars: + +Rocky planets around stars as faint as V ≈ 9 (in 1-UT mode) +Neptune-mass planets around stars as faint as V ≈ 12 (in 4-UT mode ) +Earth-size rocky planets around stars as faint as V ≈ 9 (CODEX on the E-ELT) +The best-suited candidate stars for ESPRESSO are non-active, non-rotating, quiet G dwarfs to red dwarfs. It operates at the peak of its efficiency for a spectral type up to M4-type stars. + +== Instrument == + +In the singleHR mode ESPRESSO can be fed by any of the four UTs. \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/ESPRESSO-1.md b/data/en.wikipedia.org/wiki/ESPRESSO-1.md new file mode 100644 index 000000000..c2e053e96 --- /dev/null +++ b/data/en.wikipedia.org/wiki/ESPRESSO-1.md @@ -0,0 +1,65 @@ +--- +title: "ESPRESSO" +chunk: 2/2 +source: "https://en.wikipedia.org/wiki/ESPRESSO" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:41.044146+00:00" +instance: "kb-cron" +--- + +== Status == + +All design work was completed and finalised by April 2013, with the manufacturing phase of the project commencing thereafter. ESPRESSO was tested on June 3, 2016. ESPRESSO first light occurred on September 25, 2016, during which they spotted various objects, among them the star 60 Sgr A. After being shipped to Chile, installed at the VLT, ESPRESSO saw its first light there on 27 November 2017, in 1-UT mode, observing the star Tau Ceti; the first star observed in the 4-UT mode was on February 3, 2018. +A problem was discovered in the ESPRESSO charge-coupled device controllers, digital imaging hardware, where a differential nonlinearity issue has reduced the resolution obtainable more severely than was previously feared. The ESO detector team that determined the source of the problem is currently, as of June 2019, working on a new version of the associated hardware in order to remedy this hopefully temporary setback. +On August 29, 2019, the ESPRESSO ETC was updated to reflect the gain in transmission after the technical mission of July. This gain influx was, on average, ≈50% in the UHR and HR modes and ≈40% in the MR. +As of April 6, 2020, the red radial velocity detector has, at least for a very short time, achieved the ≈10 cm/s precision, while the blue detector has so far only managed ≈60 cm/s. Due to the limited spectral coverage and lack of reliability, the Laser Frequency Comb (LFC) is currently not integrated into the telescope and for now complete wavelength calibration will have to rely on the two backup ThAr lamps, with resultant radial velocity measurements values limited by photon noise, stellar jitter and so less precise than expected. The ESPRESSO operator and detector teams are working to characterize and correct the problem, with a dedicated mission expected to take place during 2020. +On May 24, 2020, a team led by A. Suárez Mascareño confirmed the existence of the exoplanet Proxima b, finding it to be about 1.17 times the mass of Earth—smaller than the older estimate of 1.3 times. They also suggested it is located in the habitable zone of its star, which it orbits in 11.2 days. ESPRESSO achieved an accuracy of 26 cm/s, about three times the accuracy obtained with HARPS. They also found a second signal in the data that could be of planetary origin with a semi-amplitude of only 40 cm/s and a 5.15-day period. +On August 28, 2020, it was announced that in the coming weeks minimal science operations are planned to be resumed at the Paranal Observatory, following after a five-month suspension due to the COVID-19 pandemic. +As of June 11, 2021, there is still an ongoing issue with the blue cryostat detector caused by temperature instabilities, and there has been a communication problem between the Atmospheric Dispersion Corrector and the rest of the instrument, these issues are currently reducing the detection resolution achievable with the instrument. +A major instrument intervention was scheduled between May 1 and May 16, 2022, and the instrument will be out of operations between May 1 until around May 23. After the intervention, an improvement in the overall instrument performance, and in the radial velocity stability, particularly in the blue detector, is expected. +As a result of the instrument intervention the blue cryostat stability has dramatically improved. However, because of a change of the cross dispersion and dispersion direction positions (in both the x and y direction) from the red and blue cryostat detectors induced by the instrument intervention, combining data from different pixels to produce a focused image has become problematic in the MR4x2 mode and the new HR4x2 mode. This problem should be fixed in the new pipeline version, i.e. in an upcoming software update. + +== Scientific objectives == +The main scientific objectives for ESPRESSO are: + +The measurement of high precision radial velocities of solar type stars for the search for rocky planets in the habitable zone of their star. +The measurement of the variation of the physical constants +The analysis of the chemical composition of stars in nearby galaxies. + +== Consortium == +ESPRESSO was developed by a consortium consisting on the European Southern Observatory (ESO) and seven scientific institutes: + +Centre for Astrophysics of the University of Porto (Portugal) +Faculdade de Ciências da Universidade de Lisboa, CAAUL & LOLS (Portugal) +Trieste Astronomical Observatory (Italy) +Brera Astronomical Observatory (Italy) +Instituto de Astrofísica de Canarias (Spain) +Physics Institute of the University of Bern (Switzerland) +University of Geneva (Switzerland) +Institute of Astrophysics and Space Sciences (Portugal) +The principal investigator is Francesco Pepe. + +== ESPRESSO specifications == + +== Radial velocity comparison tables == + +=== MK-type stars with planets in the habitable zone === + +== See also == + +CORALIE spectrograph +Doppler spectroscopy +ELODIE spectrograph +EXPRES spectrograph +HIRES spectrograph +Lists of planets +SOPHIE échelle spectrograph + +== References == + +== External links == + Media related to ESPRESSO at Wikimedia Commons +ESPRESSO at eso.org +ESPRESSO at unige.ch Archived 2016-09-25 at the Wayback Machine +Pepe, F.; Molaro, P.; Cristiani, S.; Rebolo, R.; Santos, N. C.; Dekker, H.; Mégevand, D.; Zerbi, F. M.; Cabral, A.; Di Marcantonio, P.; Abreu, M.; Affolter, M.; Aliverti, M.; Allende Prieto, C.; Amate, M.; Avila, G.; Baldini, V.; Bristow, P.; Broeg, C.; Cirami, R.; Coelho, J.; Conconi, P.; Coretti, I.; Cupani, G.; D'Odorico, V.; De Caprio, V.; Delabre, B.; Dorn, R.; Figueira, P.; et al. (2014). "ESPRESSO: The next European exoplanet hunter". arXiv:1401.5918 [astro-ph.IM]. \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/EXPRES-0.md b/data/en.wikipedia.org/wiki/EXPRES-0.md new file mode 100644 index 000000000..c6a22eebd --- /dev/null +++ b/data/en.wikipedia.org/wiki/EXPRES-0.md @@ -0,0 +1,19 @@ +--- +title: "EXPRES" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/EXPRES" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:44.606027+00:00" +instance: "kb-cron" +--- + +The EXtreme PREcision Spectrograph (EXPRES) is an optical fiber fed echelle instrument designed and built at the Yale Exoplanet Laboratory to be installed on the 4.3-meter Lowell Discovery Telescope operated by Lowell Observatory. It has a goal to achieve 10 cm/s radial velocity precision. It uses a laser frequency comb to calibrate the primary wavelength for EXPRES. + + +== See also == +ESPRESSO spectrograph +HARPS3 + + +== References == \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Eidouranion-0.md b/data/en.wikipedia.org/wiki/Eidouranion-0.md new file mode 100644 index 000000000..f0bac5dcc --- /dev/null +++ b/data/en.wikipedia.org/wiki/Eidouranion-0.md @@ -0,0 +1,24 @@ +--- +title: "Eidouranion" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Eidouranion" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:35.019531+00:00" +instance: "kb-cron" +--- + +An eidouranion is a kind of orrery that combined mechanical movement with a method of back projection. Its invention is attributed to Adam Walker (1731–1821) who in the 1780s built one measuring 27 ft (8.2 m) in diameter. He used it to accompany his lectures on astronomy. It is an ancestor of planetarium projectors. +It is known that Adam Walker held lectures featuring the Eidouranium at the Royal Theatre in London in the 1780s and the London Lyceum. The shows were continued by his eldest son, William Walker (1767-1816), from around 1812. The shows were continued through the 1820s by William’s younger brother Deane Franklin Walker (1778-1865). +The word "eidouranion" derives from the Greek compound "eid + ouranos". The combining elements are "eidos", which means "what is seen, shape, form", and "ouranos", which was the name of the god of the heavens. Thus, the combined form means "shaped like the heavens" or "formed like the heavens". + + +== References == + + +== Further reading == +King, Henry C, and John R. Millburn. Geared to the Stars: The Evolution of Planetariums, Orreries, and Astronomical Clocks. Toronto: University of Toronto Press, 1978. Print. [esp. Ch. 19: The Eidouranion and Other Large Transparent Orreries] + + +== External links == +The Shows of London by Richard Daniel Altick, p. 364 \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Elton's_quadrant-0.md b/data/en.wikipedia.org/wiki/Elton's_quadrant-0.md index f3b4807b7..cd676d0cb 100644 --- a/data/en.wikipedia.org/wiki/Elton's_quadrant-0.md +++ b/data/en.wikipedia.org/wiki/Elton's_quadrant-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Elton's_quadrant" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:56.867994+00:00" +date_saved: "2026-05-05T09:40:37.388651+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Equatorial_ring-0.md b/data/en.wikipedia.org/wiki/Equatorial_ring-0.md index d355c6bcc..113993480 100644 --- a/data/en.wikipedia.org/wiki/Equatorial_ring-0.md +++ b/data/en.wikipedia.org/wiki/Equatorial_ring-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Equatorial_ring" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:58.041980+00:00" +date_saved: "2026-05-05T09:40:38.637038+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Equatorium-0.md b/data/en.wikipedia.org/wiki/Equatorium-0.md index 8a6de1536..51a3aeaa9 100644 --- a/data/en.wikipedia.org/wiki/Equatorium-0.md +++ b/data/en.wikipedia.org/wiki/Equatorium-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Equatorium" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:59.223473+00:00" +date_saved: "2026-05-05T09:40:39.861425+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/European_Pulsar_Timing_Array-0.md b/data/en.wikipedia.org/wiki/European_Pulsar_Timing_Array-0.md new file mode 100644 index 000000000..986ea0453 --- /dev/null +++ b/data/en.wikipedia.org/wiki/European_Pulsar_Timing_Array-0.md @@ -0,0 +1,37 @@ +--- +title: "European Pulsar Timing Array" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/European_Pulsar_Timing_Array" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:42.221887+00:00" +instance: "kb-cron" +--- + +The European Pulsar Timing Array (EPTA) is a European collaboration to combine five 100-m class radio-telescopes to observe an array of pulsars with the specific goal of detecting gravitational waves. It is one of several pulsar timing array projects in operation, and one of the four projects comprising the International Pulsar Timing Array, the others being the Parkes Pulsar Timing Array, the North American Nanohertz Observatory for Gravitational Waves, and the Indian Pulsar Timing Array. + + +== Pulsars and high-precision timing == +Pulsars are rapidly rotating, highly magnetised neutron stars that emit radio waves from their magnetic poles that are, due to the star's rotation, observed on Earth as a string of pulses. Due to the extremely high density of neutron stars, their rotation periods are very stable, hence the observed arrival time of the pulses are highly regular. These arrival times are called TOAs (time of arrival) and can be used to perform high-precision timing experiments. +The stability of the TOAs from most pulsars is limited due to the presence of red noise, also called "timing noise". However, there is a special class of pulsars, called millisecond pulsars (MSP), that are shown to suffer from little or no timing noise. Keeping track of the TOAs of different MSPs over the sky allows for a high-precision timing experiment to detect gravitational waves. + + +== Detection of gravitational waves == +Gravitational waves (GW) are small disturbances in space-time, caused by the motion of masses, if the third time derivative of the mass quadrupole moment is non-zero. These waves are very weak, such that only the strongest waves, caused by the rapid motion of dense stars or black-holes, have a chance of being detected. A pulsar timing array (PTA) uses an array of MSPs as the endpoints of a Galaxy-scale GW detector. It is sensitive to GWs with a frequency in the nanohertz regime, which corresponds to the regime where the stochastic GW background, caused by the coalescence of super-massive black holes in the early Universe, is predicted to exist. This makes PTAs complementary to other GW detectors such as LIGO, VIRGO and LISA. +The EPTA is one component of a worldwide collaboration for detecting and measuring gravitational waves, the International Pulsar Timing Array, which also includes the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) and the Parkes Pulsar Timing Array (PPTA). + + +== Telescopes == +The EPTA uses five European telescopes. These are the Westerbork Synthesis Radio Telescope, the Effelsberg Radio Telescope, the Lovell Telescope, the Nançay Radio Telescope and the Sardinia Radio Telescope. + + +== LEAP == + +Since 2009, the EPTA has made some progress thanks to a project European Research Council funded project known as the Large European Array for Pulsars (LEAP). The aim of this project is to coherently combine the five EPTA telescopes to synthesise the equivalent of a fully steerable 194-m dish. This will improve the accuracy with which the pulsar TOAs can be measured by an order of magnitude, essential for the first detection of gravitational waves within the next decade. + + +== Notes == + + +== External links == +European Pulsar Timing Array \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/ExoLife_Finder-0.md b/data/en.wikipedia.org/wiki/ExoLife_Finder-0.md new file mode 100644 index 000000000..d95f74d2c --- /dev/null +++ b/data/en.wikipedia.org/wiki/ExoLife_Finder-0.md @@ -0,0 +1,43 @@ +--- +title: "ExoLife Finder" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/ExoLife_Finder" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:43.413295+00:00" +instance: "kb-cron" +--- + +The ExoLife Finder (ELF) telescope is an under-development, hybrid interferometric telescope being designed at the Instituto de Astrofisica de Canarias (IAC) for the direct detection and imaging of exoplanets and potentially water-bearing exoplanets. Developed by a collaboration of scientists and engineers including the PLANETS Foundation, the ELF aims to analyze the surfaces and atmospheres of exoplanets for evidence of life, focusing on nearby star systems within 25 light years of Earth. The telescope's design features non-redundant circular arrays of 5-meter-scale mirrors and tensegrity-based mechanical support with an outer diameter of 35m. It uses multiple layers of advanced atmospheric wavefront sensing and control. It is a scalable optical concept, and could be built within a 10 year timeframe. A 3.5-meter precursor called the Small ELF (SELF) is currently being built in the Canary Islands. The ELF's first targets will include nearby stars cooler than the Sun. +ELF incorporates several new technologies in order to study exoplanets that could be 100 million times fainter than the stars they orbit. This combination of technologies results in smoother and lighter optics compared to conventional telescope mirrors and greater control of optical diffraction and wavefront errors created by the atmosphere. According to the team behind ELF, the telescope's imaging capabilities and detection methods, which include analyzing planetary energy signatures and spectroscopic chemical fingerprints, will advance our understanding of exoplanetary environments and the search for extraterrestrial life. + + +== The Small ELF (SELF) == +The Small ExoLife Finder (SELF) telescope is a 3.5m outer diameter Fizeau telescope built from 15 0.5m diameter subapertures arranged in a circular pattern like the ELF telescope. SELF uses a telescope support structure built from a tensegrity structure of cables and compressional elements. This structure creates a stiff basis for the optics that can be 10 times lighter than a conventional truss structure. The subapertures are aligned and carefully phased using a small secondary mirror for each of the 15 subapertures. Machine learning algorithms and photonic structures built into the optical system allow the SELF to overcome the effects of the atmosphere to suppress the bright central starlight in order to see the exoplanetary environments around nearby bright stars. + + +== Laboratory for Innovation in OptoMechanics (LIOM) == +The key to finding life is to measure reflected starlight from an exoplanet. ELF does this with a very large diameter telescope using optical technologies that can measure and correct the distortions in the optical wavefront created by the atmosphere above the telescope and the telescope's imperfections. The ELF depends on 4 innovations: 1) new ways of creating accurate light-weight large mirrors without grinding glass, 2) a scalable optical system that combines elements of conventional telescopes with interferometry, 3) new ways of precisely supporting optics without massive mechanical trusses, and 4) photonics and machine learning innovations to measure and correct the stellar wavefront. IAC hosts the Laboratory for Innovation in OptoMechanics (LIOM) where scientists, engineers, and students are working on solving all of these problems. + + +== Design and specifications == +The ExoLife Finder (ELF) is a specialized large telescope designed for exoplanetary research, with an ultimate focus on detecting the energy signatures of life or its optical fingerprints on nearby exoplanets. The ELF is effectively a Fizeau interferometer that links an array of diffraction-limited unobscured off-axis subaperture telescopes at a common Gregorian focus. The direct detection of exoplanetary light relies on an extremely large telescope aperture with superior control of diffraction and correction of atmospheric wavefront distortions. The ELF's basic design consists of circular arrays of 5-meter-scale mirrors, utilizing thin curvature-polished technology, resulting in a total diameter of about 35 meters. This size allows the ELF to "image" dozens of exoplanets within 25 light years of Earth, opening a new window onto exoplanetary science and the search for extraterrestrial life. +Cost is highly dependent on system mass and the ELF employs a structural principle called tensegrity which utilizes actively controlled tension and compression to greatly reduce weight. Tensegrity is often used in bridge designs but the term originated with Buckminster Fuller 50 years ago. Each of the ELF's mirrors has a dedicated secondary off-axis mirror. Off-axis telescopes are often used in radio dish receivers, but their usage in optical telescopes has been made possible by new polishing technology. This design reduces scattered light that might interfere with the faint optical signal received from exoplanets. +The ELF is intended to be scalable, affordable, and rapidly buildable within a decade timeframe. Its unusual design allows the telescope to achieve the sensitivity needed to reconstruct images of exoplanets, making it the earliest and most cost-effective path forward for finding and characterizing life on nearby exoplanets. + + +=== Mirror technology === +One of the key innovations of the ELF telescope is its mirror technology, which significantly differs from that of traditional telescopes that are descended from the abrasive glass shaping concept pioneered by Isaac Newton 500 years ago. Such traditional telescope mirrors are several centimeters thick and can require many 10's of cycles of rubbing and measuring to achieve a high quality optical surface. Large optical mirrors like these typically cost $0.5M per m2. The combination of curvature polishing and tensegrity support structures can reduce the cost and time to fabricate large telescope optics by more than an order of magnitude. Dynamically maintaining the shape of such thin mirrors against gravity direction changes and wind forces is done with 3D printed electroactive polymers. + + +=== Imaging and detection capabilities === +ELF is designed to indirectly image the surface of exoplanets and to detect the energy signatures and spectroscopic chemical fingerprints that are indicative of life. The telescope's primary focus is on detecting molecules such as water, oxygen, methane, carbon dioxide, and ozone, which are commonly associated with life on Earth. Additionally, the ELF is capable of detecting photosynthetic bio-pigments on the surface of exoplanets, which could indicate the presence of photosynthetic organisms. +The ELF's useful imaging capabilities extend up to 120 trillion miles, or 24 light years, away from Earth with a particular sensitivity for exoplanets around stars cooler than the Sun. This range allows it to target dozens of exoplanets within 25 light years of the Solar System, including the nearby star system Alpha Centauri, which holds promising worlds like Proxima B in the habitable zone. +To achieve its imaging and detection goals, the ELF utilizes the so-called vortex nulling properties of its Fizeau interferometry. These optics create what is called a coronagraph from the telescope primary optics alone. The use of complex inversion algorithms that depend on repeated observations of the exoplanet systems over months then samples the exoplanetary rotation and orbit to reveal details of its surface structure like oceans, continents, forests, deserts, or even city complexes. + + +== Location == +The precursor small ELF is locate on Mt. Teide on Tenerife island and the proposed location for the full ELF telescope could be in the Canary Islands for seeing the Northern sky or in Chile's Atacama Desert to see southern exoplanets like Proxima B. The remote and dry environment of the Atacama Desert provides optimal conditions for astronomical observations, while minimizing light pollution and atmospheric disturbances. + + +== References == \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Fiber-optic_Improved_Next-generation_Doppler_Search_for_Exo-Earths-0.md b/data/en.wikipedia.org/wiki/Fiber-optic_Improved_Next-generation_Doppler_Search_for_Exo-Earths-0.md new file mode 100644 index 000000000..75f6f988a --- /dev/null +++ b/data/en.wikipedia.org/wiki/Fiber-optic_Improved_Next-generation_Doppler_Search_for_Exo-Earths-0.md @@ -0,0 +1,25 @@ +--- +title: "Fiber-optic Improved Next-generation Doppler Search for Exo-Earths" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Fiber-optic_Improved_Next-generation_Doppler_Search_for_Exo-Earths" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:45.746135+00:00" +instance: "kb-cron" +--- + +The Fiber-Optic Improved Next-Generation Doppler Search for Exo-Earths (FINDS Exo-Earths) is a radial-velocity spectrograph developed by Debra Fischer. It is installed on the 3 meter telescope in Lick Observatory in Mount Hamilton. It has been in operation since 2009 and is being used to verify exoplanet candidates found by the Kepler space telescope. +At Yale University, Debra Fischer and Julien Spronck, along with Geoff Marcy of the University of California, Berkeley, set out to improve existing spectrograph technologies. Spurred by a $45,000 grant from The Planetary Society, the team built FINDS, a spectrograph add-on device. + + +== See also == +List of potentially habitable exoplanets +Similar instruments +CORALIE spectrograph +ELODIE spectrograph, the precursor instrument +ESPRESSO, a new-generation spectrograph for ESO's VLT +HARPS +SOPHIE échelle spectrograph + + +== References == \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Filar_micrometer-0.md b/data/en.wikipedia.org/wiki/Filar_micrometer-0.md index d5198d2b8..6def30101 100644 --- a/data/en.wikipedia.org/wiki/Filar_micrometer-0.md +++ b/data/en.wikipedia.org/wiki/Filar_micrometer-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Filar_micrometer" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:37:01.632726+00:00" +date_saved: "2026-05-05T09:40:46.991471+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/GRAVITY_(Very_Large_Telescope)-0.md b/data/en.wikipedia.org/wiki/GRAVITY_(Very_Large_Telescope)-0.md new file mode 100644 index 000000000..6e2f9cbde --- /dev/null +++ b/data/en.wikipedia.org/wiki/GRAVITY_(Very_Large_Telescope)-0.md @@ -0,0 +1,36 @@ +--- +title: "GRAVITY (Very Large Telescope)" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/GRAVITY_(Very_Large_Telescope)" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:53.008414+00:00" +instance: "kb-cron" +--- + +GRAVITY is an instrument on the interferometer of the Very Large Telescope (VLTI). It either combines the light of the four Unit Telescopes (UT) or the smaller four Auxiliary Telescopes. The instrument works with adaptive optics and provides a resolution of 4 milliarcseconds (mas) and can measure the position of astronomical objects down to a few 10 microarcseconds (μas). VLTI GRAVITY has a collecting area of 200 m2 and the angular resolution of a 130 m telescope. + + +== Instrument details == +GRAVITY was built by a consortium led by the Max Planck Institute for Extraterrestrial Physics. Other partner institutes are from France, Germany, Portugal and the European Southern Observatory. The first light images included the discovery that Theta1 Orionis F in the Trapezium Cluster is a binary. +GRAVITY can operate in single-field mode or in dual-field mode. In the dual-field mode it can interfere two astronomical objects at the same time and acquire this way very accurate astrometry. The instrument data can also be used for K-band spectroscopy with three spectral resolutions. GRAVITY has the following sub-components: + +IR wavefront sensing system CIAO (located at the Unit Telescopes) that will work with the MACAO deformable mirror +A polarisation control system to counteract polarisation effects in the VLTI +An active pupil guide system including LED sources mounted on each of the telescope secondary mirror support (spiders) +A field-guide system to track the position of the source +The Beam Combining Instrument (BCI) +The Beam Combining Instrument is the primary unit of GRAVITY. It performs acquisition and provides interferometric fringes. BCI is cryogenically cooled and located in the VLT-I laboratory. + + +== Science == + +GRAVITY is mainly used to observe the stars orbiting the supermassive black hole Sagittarius A* and the position of exoplanets and brown dwarfs around their host star. It is also used for other studies that require a high resolution, such as the study of circumstellar disks and the study of AGNs. + + +== GRAVITY+ == + +GRAVITY+ is the upgrade of GRAVITY, which will increase its sensitivity and increase its sky coverage. The upgrade is performed incrementally to reduce the disruption of astronomical observations. GRAVITY+ or Gravity Plus Adaptive Optics (GPAO) had first light at the end of 2024, by using natural guide stars (NGS) to observe targets. Part of the upgrade was the equipment of all four Unit Telescopes with AO systems. The observations included a sub-microarcsecond differential astrometry of β Pictoris, which showed that the stellar rotation axis is aligned with the warped inner disk and not with the outer disk. + + +== References == \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Giant_Radio_Array_for_Neutrino_Detection-0.md b/data/en.wikipedia.org/wiki/Giant_Radio_Array_for_Neutrino_Detection-0.md new file mode 100644 index 000000000..58bc276f9 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Giant_Radio_Array_for_Neutrino_Detection-0.md @@ -0,0 +1,37 @@ +--- +title: "Giant Radio Array for Neutrino Detection" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Giant_Radio_Array_for_Neutrino_Detection" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:48.179050+00:00" +instance: "kb-cron" +--- + +The Giant Radio Array for Neutrino Detection (GRAND) is a proposed large-scale detector designed to collect ultra-high energy cosmic particles as cosmic rays, neutrinos and photons with energies exceeding 1017 eV. This project aims at solving the mystery of their origin and the early stages of the universe itself. The proposal, formulated by an international group of researchers, calls for an array of 200,000 receivers to be placed on mountain ranges around the world. + + +== Overview == +The GRAND detector would search for neutrinos, exotic particles emitted by some and the black holes in the center of galaxies. These neutrinos could help astronomers find the source of other energetic particles called ultra-high-energy cosmic rays. When neutrinos reach Earth, they often collide with particles either in the air or on the ground, creating showers of secondary particles. These secondary particles can be picked up by the radio antennas, which lets researchers calculate the trajectory of the initial neutrinos and trace them back to their source. The concept was first published in 2017. +The giant radio detector array would comprise 200,000 low-cost antennas in groups of 10,000 spread out over nearly 200,000 square kilometres (77,000 sq mi) at different locations around the world. This would make it the largest detector in the world. Construction, installation and networking the 200,000 antennae, would cost approximately US$226 million, excluding the price for renting the land and manpower. + + +== Principle == +The strategy of GRAND is to detect the radio emission coming from particle showers that develop in the terrestrial atmosphere as a result of the interaction of ultra-high energy (UHE) cosmic rays, gamma rays, and neutrinos. Astrophysical tau neutrinos (ντ) can be detected through extensive air showers (EAS) induced by tau (τ−) decays in the atmosphere. The short-lived tau decays in the atmosphere generates an EAS that emits measurable electromagnetic emissions up to frequencies of hundreds of MHz. The antennae are foreseen to operate in the 60-200 MHz band to avoid the short-wave background noise at lower frequencies. +Each individual antenna is a simple Bow-tie design, featuring 3 perpendicular bows with an additional vertical arm to sample all three polarization directions. Each antenna is mounted on a single 5-meter-tall pole, and each antenna in the grid is spaced at 1 km within a square grid. If the full array of 200,000 antennae is built, GRAND would reach an all-flavor sensitivity of 4 ×10−10 GeV cm−2 s−1 sr−1 above 5 ×1017 eV. Because of its sub-degree angular resolution, GRAND will also search for point sources of UHE neutrinos, steady and transient, potentially starting UHE neutrino astronomy, allowing for the discovery and follow-up of large numbers of radio transients, fast radio bursts, giant radio pulses, and for precise studies of the epoch of reionization. +The researchers estimate that GRAND could allow not just the detection of neutrinos, but could also allow a differentiation of the source types, such as galaxy clusters with central sources, fast-spinning newborn pulsars, active galactic nuclei, and afterglows of gamma-ray bursts. + + +== Status == +Simulation and experimental work is ongoing on technological development and background rejection strategies. Phase one is called GRANDProto35, that includes 35 antennas and 24 scintillators, deployed in the Tian Shan mountains in China. If a pulse is observed simultaneously in the signals from three or more scintillators, the signals are recorded. As of October 2018, GRANDProto35 is in commissioning phase. So far, the system achieves 100% detection efficiency for trigger rates up to 20 kHz. +The following step is planned for 2020, and it is a dedicated setup called GRANDProto300 within an area of 300 square kilometres (120 sq mi). The baseline layout is a square grid with a 1 kilometre (0.62 mi) inter-antenna spacing, just as for later stages. Because GRANDProto300 will not be large enough to detect cosmogenic neutrinos, the viability will be tested using instead extensive air showers initiated by very inclined cosmic rays, thus providing an opportunity to do cosmic-ray science. The site would be hosted at the Chinese provinces of XinJiang, Inner Mongolia, Yunnan, and Gansu. If funded, the later phases would build GRAND10k in 2025, and finally GRAND200k (200,000 receivers) in the 2030s. + + +== See also == +High-energy astronomy +List of neutrino experiments +Multi-messenger astronomy +Neutrino astronomy + + +== References == \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Globe_of_Matelica-0.md b/data/en.wikipedia.org/wiki/Globe_of_Matelica-0.md index ecbf4dcc6..6f9b1fac5 100644 --- a/data/en.wikipedia.org/wiki/Globe_of_Matelica-0.md +++ b/data/en.wikipedia.org/wiki/Globe_of_Matelica-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Globe_of_Matelica" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:38:42.195626+00:00" +date_saved: "2026-05-05T09:40:49.395028+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Gnomon-0.md b/data/en.wikipedia.org/wiki/Gnomon-0.md new file mode 100644 index 000000000..322163a38 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Gnomon-0.md @@ -0,0 +1,72 @@ +--- +title: "Gnomon" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Gnomon" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:50.565275+00:00" +instance: "kb-cron" +--- + +A gnomon (; from Ancient Greek γνώμων (gnṓmōn) 'one that knows or examines') is the part of a sundial that casts a shadow. The term is used for a variety of purposes in mathematics and other fields, typically to measure directions, position, or time. + + +== History == + +A painted stick dating from 2300 BC that was excavated at the archeological site of Taosi is the oldest gnomon known in China. The gnomon was widely used in ancient China from the second millennium BC onward in order to determine the changes in seasons, orientation, and geographical latitude. The ancient Chinese used shadow measurements for creating calendars that are mentioned in several ancient texts. +According to the collection of Zhou Chinese poetic anthologies Classic of Poetry, one of the distant ancestors of King Wen of the Zhou dynasty used to measure gnomon shadow lengths to determine the orientation around the 14th century BC. +The ancient Greek philosopher Anaximander (610–546 BC) is credited with introducing this Babylonian instrument to the Ancient Greeks. +The ancient Greek mathematician and astronomer Oenopides used the phrase drawn gnomon-wise to describe a line drawn perpendicular to another. Later, the term was used for an L-shaped instrument like a steel square used to draw right angles. This shape may explain its use to describe a shape formed by cutting a smaller square from a larger one. Euclid extended the term to the plane figure formed by removing a similar parallelogram from a corner of a larger parallelogram. Indeed, the gnomon is the increment between two successive figurate numbers, including square and triangular numbers. + + +=== Definition of Hero of Alexandria === +The ancient Greek mathematician and engineer Hero of Alexandria defined a gnomon as that which, when added or subtracted to an entity (number or shape), makes a new entity similar to the starting entity. In this sense Theon of Smyrna used it to describe a number which added to a polygonal number produces the next one of the same type. The most common use in this sense is an odd integer especially when seen as a figurate number between square numbers. + + +=== Vitruvius === +Vitruvius mentions the gnomon as "gnonomice" in the first sentence of chapter 3 in volume 1 of his book De Architectura. That Latin term "gnonomice" leaves room for interpretation. Despite its similarity to "γνωμονικός" (or its feminine form "γνωμονική"), it appears unlikely that Vitruvius refers to judgement on the one hand or to the design of sundials on the other. It appears to be more appropriate to assume that he refers to geometry, a science upon which gnomons rely heavily. In those days, calculations were carried out geometrically, in contrast to the algebraic methods in use today. Thus, it seems that he indirectly refers to mathematics and geodesy. + + +== Pinhole gnomons == + +Perforated gnomons projecting a pinhole image of the Sun whose location can be measured to tell the time of day and year were described in the Chinese Zhoubi Suanjing, possibly dating as early as the early Zhou (11th century BC) but surviving only in forms dating to the Eastern Han (3rd century). +In the Middle East and Europe, it was separately credited to the Egyptian astronomer and mathematician Ibn Yunus around AD 1000. The Italian astronomer, mathematician and cosmographer Paolo Toscanelli is associated with the 1475 placement of a bronze plate with a round hole in the dome of the Cathedral of Santa Maria del Fiore in Florence to project an image of the Sun on the cathedral's floor. With markings on the floor it tells the exact time of each midday (reportedly to within half a second) as well as the date of the summer solstice. Italian mathematician, engineer, astronomer and geographer Leonardo Ximenes reconstructed the gnomon according to his new measurements in 1756. + + +== Orientation == + +In the Northern Hemisphere, the shadow-casting edge of a sundial gnomon is normally oriented so that it points due northward and is parallel to the rotational axis of Earth. That is, it is inclined to the northern horizon at an angle that equals the latitude of the sundial's location. At present, such a gnomon should thus point almost precisely at Polaris, as this is within 1° of the north celestial pole. +On some sundials, the gnomon is vertical. These were usually used in former times for observing the altitude of the Sun, especially when on the meridian. + + +=== Style === +The style is the part of the gnomon that casts the shadow. This can change as the Sun moves. For example, the upper west edge of the gnomon might be the style in the morning and the upper east edge might be the style in the afternoon. + + +== Modern uses == + +Gnomons have been used in space missions to the Moon and Mars. The gnomon used by the Apollo astronauts was a gimballed stadia rod mounted on a tripod. While the rod's shadow indicated the direction of the Sun, the grayscale paints of varying reflectivity and the red, green and blue patches facilitated proper photography on the surface on the Moon. MarsDials have been used on Mars Exploration Rovers. + + +== In computer graphics == + +A three-dimensional gnomon is commonly used in CAD and computer graphics as an aid to positioning objects in the virtual world. By convention, the x-axis direction is colored red, the y-axis green and the z-axis blue. + + +== In popular culture == +The Gnomon of Saint-Sulpice inside the Parisian church, Église Saint-Sulpice, built to assist in determining the date of Easter, was fictionalized as a "Rose Line" in the novel The Da Vinci Code. + + +== Literary uses == +In modern literary and theoretical thought, the gnomon has been reappropriated as an epistemological and aesthetic figure, extending beyond its classical astronomical or geometrical uses. Within the contexts of modernism and postmodernism, the gnomon appears in the work of authors and thinkers such as James Joyce, Paul Valéry, Julia Kristeva, Fernand Deligny, and Michel Deguy, where it functions as a mediation between the sensible and the conceptual. Drawing on the literary work of French novelist Nathalie Sarraute, the feminist writer Monique Wittig proposed the concept of the “modern gnomon” to describe the relationship between knowledge and poetic invention. + + +== Footnotes == + + +== References == +Gazalé, Midhat J. Gnomons, from Pharaohs to Fractals, Princeton University Press, Princeton, 1999. ISBN 0-691-00514-1. +Heath, Thomas Little (1981), A History of Greek Mathematics, Dover publications, ISBN 9780486240732 (first published 1921). +Laërtius, Diogenes, The Lives and Opinions of Eminent Philosophers, trans. C.D. Yonge. London: Henry G. Bohn, 1853. +Mayall, R. Newton; Mayall, Margaret W., Sundials: Their Construction and Use, Dover Publications, Inc., 1994, ISBN 0-486-41146-X +Waugh, Albert E., Sundials: Their Theory and Construction, Dover Publications, Inc., 1973, ISBN 0-486-22947-5. \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Gnomon_of_Saint-Sulpice-0.md b/data/en.wikipedia.org/wiki/Gnomon_of_Saint-Sulpice-0.md new file mode 100644 index 000000000..1511063da --- /dev/null +++ b/data/en.wikipedia.org/wiki/Gnomon_of_Saint-Sulpice-0.md @@ -0,0 +1,43 @@ +--- +title: "Gnomon of Saint-Sulpice" +chunk: 1/2 +source: "https://en.wikipedia.org/wiki/Gnomon_of_Saint-Sulpice" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:51.817571+00:00" +instance: "kb-cron" +--- + +The Gnomon of Saint-Sulpice is an astronomical measurement device located in the Church of Saint-Sulpice (Église Saint-Sulpice) in Paris, France. It is a gnomon, a device designed to cast a shadow on the ground in order to determine the position of the sun in the sky. In early modern times, other gnomons were also built in several Italian and French churches in order to better calculate astronomical events. Those churches are Santa Maria del Fiore in Florence, San Petronio in Bologna, and the Church of the Certosa in Rome. These gnomons ultimately fell into disuse with the advent of powerful telescopes. + +== Structure == + +The gnomon of Saint-Sulpice is composed of different parts that span the breadth of the transept of the church. The church itself is a huge building, the largest church in Paris. +The system is first built around a meridian, a line which is strictly oriented along the north-south axis, represented by a brass line set in a strip of white marble on the floor of the church. This is not the Paris Meridian, established by Louis XIV in 1667, which is located a few hundred metres to the east and goes through the Paris Observatory. + +The sunlight passes through a small round opening in the southern stained-glass window of the transept, at a height of 25 metres, forming a small light disc on the floor; this disc will cross the meridian each time the sun reaches its zenith at true noon. The sun will cross different parts of the meridian depending the time of year, as the sun will be more or less high in the sky at noon. A point on the meridian is marked with a gold disc which shows the position of the sun at an equinox. It is located right in front of the altar. +At one end of the meridian is a square marble plaque, which corresponds to the position of the sun at the highest at midday (64°35' at the location of Saint-Sulpice), during the summer solstice about 21 June. +At the other end is an obelisk, which is lit near its top when the sun is at it lowest at midday (17°42' at the location of Saint-Sulpice). If the obelisk did not exist, the sun disc would hit an area about 20 metres beyond the wall of the church. + +== Usage of the gnomon == +The gnomon was built at the initiative of Jean-Baptiste Languet de Gergy, the parish priest at Saint-Sulpice from 1714 to 1748. Languet de Gergy initially wished to establish the exact astronomical time in order to ring the bells at the most appropriate time of day. For this, he commissioned the English clockmaker Henry Sully to build the gnomon. + +The gnomon could also have been used to properly time clocks by properly defining mean time. Mean time (the time used in clocks) is only an average of true time (the time deduced from the apparent motions of the Sun in the sky, and shown, approximately, by a sundial). True time deviates from the mechanical average of a clock by as much as +/-16 minutes throughout the year. These variations are codified in the equation of time. Henry Sully, however, died in 1728 without being able to accomplish this larger project. He was only able to set the meridian line in the floor of the Church. The project was completed by the nearby Paris Observatory a year later. + +=== Computation of official time === +The time the sun disk crosses the Saint-Sulpice meridian gives the "true" local midday at that place. In order to compute the official French time from this, it is necessary to: + +add or subtract the deviation given by the equation of time. +add half a second to have the mean Paris time. +add 50 minutes 39 seconds to obtain Central European Time. +add one hour in summer to take into account daylight saving time. +Alternatively, a simpler solution would be to consult an almanac giving the time of sunrise and sundown, calculate the middle point of that time-span, corresponding to the maximum elevation of the sun. This gives the official time at which the sun reaches it maximum elevation, and therefore the time the sun disk crosses the Saint-Sulpice meridian. + +=== Computation of the Paschal equinox === + +After this first attempt, Languet de Gergy resumed the project in 1742, this time with the objective of properly defining the Easter Equinox. The task was given to Pierre Charles Le Monnier, member of the French Academy of Sciences. + +The inscription at the base of the obelisk mentions Charles Claude Le Monnier, as well as the mission of the gnomon in Latin: "Ad Certam Paschalis Æquinoctii Explorationem" ("To determine precisely the Paschal Equinox"). +The dating of Easter was modeled on that of the Jewish Passover, which marks the liberation of the Jews from Egypt and which traditionally falls in the Jewish lunar calendar on the 14th of the month of Nisan, the day of the first full moon after the vernal (spring) equinox. Roman Christians, however, had a twelve-month calendar, first the Julian calendar until 1582, and then the Gregorian calendar. Since the Council of Nicaea in 325, the Western Church had required that Easter be celebrated on the Sunday on or after the full moon following March 21, which at that time corresponded indeed to the vernal equinox. The Julian calendar being imprecise however, by the 16th century March 21 fell about 10 days after the vernal equinox, a problem that was solved by the introduction of the Gregorian calendar. (The Eastern Christian Church continues to date Easter by the Julian calendar.) Languet de Gergy, however, wished to verify independently the exact date of the vernal equinox through the gnomon in order to ascertain the date of Easter. + +=== Obliquity of the ecliptic === \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Gnomon_of_Saint-Sulpice-1.md b/data/en.wikipedia.org/wiki/Gnomon_of_Saint-Sulpice-1.md new file mode 100644 index 000000000..afe0baa29 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Gnomon_of_Saint-Sulpice-1.md @@ -0,0 +1,32 @@ +--- +title: "Gnomon of Saint-Sulpice" +chunk: 2/2 +source: "https://en.wikipedia.org/wiki/Gnomon_of_Saint-Sulpice" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:51.817571+00:00" +instance: "kb-cron" +--- + +Le Monnier further used the gnomon from 1744 to establish the variations of the ecliptic, or the variations in the obliquity of the Earth's axis. The endeavour is recorded on the plaque at the southern end of the meridian, in the South transept: "Pro nutatione axios terren. obliquitate eclipticae" ("for the nutation of the earth's axis and the obliquity of the ecliptic"). +As mentioned on a brass plaque that covered the stone plaque, the obliquity of the ecliptic was 23°28'40".69 in 1744. From 1745 to 1791, Le Monnier visited Saint-Sulpice at each summer solstice and, focusing the light with a lens fixed to the opening in the stained-glass window so as to produce a sharp image of the sun on the floor, noted the exact position of the image at noon. From these observations, he calculated a variation of the obliquity of 45" per century (the exact figure is 46".85 per century). + +=== Perihelion === +The gnomon also permitted the determination of the date of the earth's perihelion (the moment the earth is closest to the sun in its elliptical trajectory around the sun), by measuring the size of the image of the sun cast on the obelisk and finding the time when it was largest. Perihelion occurs close to the winter solstice, during the period of the year when the sun's image at noon is on the obelisk, rather than on the floor of the church. + +== Interpretations == + +Some interpretations of the gnomon at Saint-Sulpice give it an occult meaning. The author Dan Brown in The Da Vinci Code describes it as "a pagan astronomical instrument (...) an ancient sundial of sorts, vestige of the pagan temple that had once stood on this very spot", despite an early modern building date of 1714, and the fact that it is an astronomical device with nothing especially pagan about it. Brown also qualifies the obelisk as "Egyptian" despite its recent date of manufacture in 1743: "a most unexpected structure, a colossal Egyptian obelisk". He also equates the Saint-Sulpice meridian with the Paris Meridian, although they are different, being several hundred meters apart: "Long before the establishment of Greenwich as the prime meridian, the zero longitude had passed through Paris and through the Church of Saint-Sulpice". +The building of the gnomon inside the Church of Saint-Sulpice occurred at a time when Rome was relaxing its stance against the theories of Galileo Galilei, as his works were being printed in Rome with the agreement of the Holy See, and in 1757 the Pope removed the works of Galileo from the Index Librorum Prohibitorum. + +== Santa Maria degli Angeli e dei Martiri == +A similar gnomon built to calculate the exact date of Easter also exists in the Santa Maria degli Angeli e dei Martiri in Rome. Commissioned by Pope Clement XI, it was designed by +Francesco Bianchini and completed in 1702. + +== See also == +Astronomical clock + +== Notes == + +== References == +Rougé, Michel The Gnomon of the Church of Saint-Sulpice, Church of Saint-Sulpice, Paris, 2009. \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Greenland_Telescope-0.md b/data/en.wikipedia.org/wiki/Greenland_Telescope-0.md new file mode 100644 index 000000000..4dbafbbc5 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Greenland_Telescope-0.md @@ -0,0 +1,37 @@ +--- +title: "Greenland Telescope" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Greenland_Telescope" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:54.149890+00:00" +instance: "kb-cron" +--- + +The Greenland Telescope is a radio telescope situated at the Pituffik Space Base in north-western Greenland. It will later be deployed at the Summit Station research camp, located at the highest point of the Greenland ice sheet at an altitude of 3,210 meters (10,530 feet). +The telescope is an international collaboration between: + +The Academia Sinica Institute of Astronomy and Astrophysics (Taiwan) (project leaders) +The Smithsonian Astrophysical Observatory of the Center for Astrophysics | Harvard & Smithsonian (United States) +The National Radio Astronomy Observatory (United States) +The Haystack Observatory of the Massachusetts Institute of Technology (United States) +In 2011 the U.S. National Science Foundation gave the Smithsonian Astrophysical Observatory a 12-meter radio antenna that had been used as a prototype for the ALMA project in Chile. The antenna was to be deployed in Greenland. Deploying the telescope in the middle of Greenland is ideal for detecting certain radio frequencies. +The telescope will be used to study the event horizons of black holes and to test how general relativity behaves in environments with extreme gravity. +The Greenland Telescope will become part of the global network of telescopes that makes up the Event Horizon Telescope that will study supermassive black holes and explore the origin of the relativistic jet in the active galaxy Messier 87. + + +== Progress and current status == + +Between 2013 and 2015, the Taiwanese Academia Sinica Institute of Astronomy and Astrophysics modified the telescope so that it would better work in the cold environment of the Arctic. The telescope was shipped to Greenland in July 2016 and re-assembled in July 2017 at Thule Air Base in north-western Greenland. The telescope took its first image on 25th of December 2017. +An update on "Construction, Commissioning, and Operations" of the telescope at Pituffik Space Base (the revised name for the complex) was published on ArXiv in July 2023, describing "the lessons learned from the operations in the Arctic regions, and the prospect of the telescope." One of the systems tested was the location system; when the telescope is deployed on the ice cap summit, it will move with the ground it is mounted on. Establishing the telescope's geographical position to the required accuracy of 5m required about an hour of observation time. The snow and ice removal systems were also successfully tested. +The telescope will be deployed at the Summit Station research camp, located at the highest point of the Greenland ice sheet. + + +== References == + + +== Additional sources == +Hirashita, Hiroyuki; Koch, Patrick M.; Matsushita, Satoki; Takakuwa, Shigehisa; Nakamura, Masanori; Asada, Keiichi; Liu, Hauyu Baobab; Urata, Yuji; Wang, Ming-Jye; Wang, Wei-Hao; Takahashi, Satoko; Tang, Ya-Wen; Chang, Hsian-Hong; Huang, Kuiyun; Morata, Oscar; Otsuka, Masaaki; Lin, Kai-Yang; Tsai, An-Li; Lin, Yen-Ting; Srinivasan, Sundar; Martin-Cocher, Pierre; Pu, Hung-Yi; Kemper, Francisca; Patel, Nimesh; Grimes, Paul; Huang, Yau-De; Han, Chih-Chiang; Huang, Yen-Ru; Nishioka, Hiroaki; Lin, Lupin Chun-Che; Zhang, Qizhou; Keto, Eric; Burgos, Roberto; Chen, Ming-Tang; Inoue, Makoto; Ho, Paul T. P.. "First-generation science cases for ground-based terahertz telescopes". Publications of the Astronomical Society of Japan, 2016: Volume 68, Issue 1, id.R1 pp. doi:10.1093/pasj/psv115 10.1093/pasj/psv115 +The M87 Workshop: Towards the 100th Anniversary of the Discovery of Cosmic Jets +Urata, Yuji; Huang, Kuiyun; Asada, Keiichi; Hirashita, Hiroyuki; Inoue, Makoto; Ho, Paul T. P. (2015). "A New Era of Submillimeter GRB Afterglow Follow-Ups with the Greenland Telescope". Advances in Astronomy. 2015 165030. arXiv:1503.07594. Bibcode:2015AdAst2015E..12U. doi:10.1155/2015/165030. +Arctic Greenland Telescope Opens New Era of Astronomy SpaceRef, 2018-05-31. \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Groombridge_Transit_Circle-0.md b/data/en.wikipedia.org/wiki/Groombridge_Transit_Circle-0.md new file mode 100644 index 000000000..fd71ef800 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Groombridge_Transit_Circle-0.md @@ -0,0 +1,24 @@ +--- +title: "Groombridge Transit Circle" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Groombridge_Transit_Circle" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:55.336144+00:00" +instance: "kb-cron" +--- + +Groombridge Transit Circle was a meridian transit circle made by Edward Troughton for the English astronomer Stephen Groombridge in 1806, which Groombridge used to compile data for the star catalogue, Catalogue of Circumpolar Stars. The advantage of a transit circle over a mural circle (which can measure polar distances) is that it allows measuring right ascension and declination at the same time. +It had an aperture of 3.5 inches and a 5-foot focal length, mounted inside two 4 foot circles on stone piers. Groombridge used the instrument to determine the positions of over 4000 circumpolar stars. +It was eventually bought by James South, and it remained at his observatory at Kensington until 1870. + + +== See also == +Groombridge 1830 + + +== References == + + +== Further reading == +Royal Institution of Great Britain (1823). The Quarterly Journal. Vol. 16. John Murray. p. 189. \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/HARPS-N-0.md b/data/en.wikipedia.org/wiki/HARPS-N-0.md new file mode 100644 index 000000000..71c1b164e --- /dev/null +++ b/data/en.wikipedia.org/wiki/HARPS-N-0.md @@ -0,0 +1,34 @@ +--- +title: "HARPS-N" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/HARPS-N" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:56.481872+00:00" +instance: "kb-cron" +--- + +HARPS-N, the High Accuracy Radial velocity Planet Searcher for the Northern hemisphere is a high-precision radial-velocity spectrograph, installed at the Italian Telescopio Nazionale Galileo, a 3.58-metre telescope located at the Roque de los Muchachos Observatory on the island of La Palma, Canary Islands, Spain. +HARPS-N is the counterpart for the Northern Hemisphere of the similar HARPS instrument installed on the ESO 3.6 m Telescope at La Silla Observatory in Chile. It allows for planetary research in the northern sky which hosts the Cygnus and Lyra constellations. In particular it allows for detailed follow up research to Kepler mission planet candidates, which are located in the Cygnus constellation region. +The instrument's main scientific goals are the discovery and characterization of terrestrial super-Earths by combining the measurements using transit photometry and doppler spectroscopy which provide both, the size and mass of the exoplanet. Based on the resulting density, rocky (terrestrial) Super-Earths can be distinguished from gaseous exoplanets. +The HARPS-N Project is a collaboration between the Geneva Observatory (lead), the Center for Astrophysics in Cambridge (Massachusetts), the Universities of St. Andrews and Edinburgh, the Queen's University Belfast, the UK Astronomy Technology Centre and the Italian Istituto Nazionale di Astrofisica. + + +== First light on sky == +First light on sky was obtained by HARPS-N on March 27, 2012, and official operations started on August 1, 2012. + + +== See also == +ESPRESSO +Euler Telescope +Geneva Extrasolar Planet Search +Next-Generation Transit Survey +SuperWASP + + +== References == + + +== External links == +Official web page of the HARPS-N Project +HARPS-N page in the TNG web site \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Helioscope-0.md b/data/en.wikipedia.org/wiki/Helioscope-0.md new file mode 100644 index 000000000..800e1fe9a --- /dev/null +++ b/data/en.wikipedia.org/wiki/Helioscope-0.md @@ -0,0 +1,24 @@ +--- +title: "Helioscope" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Helioscope" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:57.686550+00:00" +instance: "kb-cron" +--- + +A helioscope is an instrument used in observing the Sun and sunspots. +The helioscope was first used by Benedetto Castelli (1578–1643) and refined by Galileo Galilei (1564–1642). The method involves projecting an image of the sun onto a white sheet of paper suspended in a darkened room with the use of a telescope. +The first machina helioscopica or helioscope was designed by Christoph Scheiner (1575 –1650) to assist his sunspot observations. +In the context of modern astroparticle physics, the term helioscope can also refer to an experiment that seeks to observe hypothetical particles (such as the axion) produced inside the sun. Examples of such helioscope experiments searching for axions include the CERN Axion Solar Telescope and International Axion Observatory. + + +== See also == +Solar telescope +Heliometer +Spectroheliograph +Spectrohelioscope + + +== References == \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Herschel_wedge-0.md b/data/en.wikipedia.org/wiki/Herschel_wedge-0.md new file mode 100644 index 000000000..0b1db1801 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Herschel_wedge-0.md @@ -0,0 +1,31 @@ +--- +title: "Herschel wedge" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Herschel_wedge" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:58.849028+00:00" +instance: "kb-cron" +--- + +A Herschel wedge or Herschel prism is an optical prism used in solar observation to refract most of the light out of the optical path, allowing safe visual observation. It was first proposed and used by astronomer John Herschel in the 1830s. + + +== Overview == +The prism in a Herschel wedge has a trapezoidal cross section. The surface of the prism facing the light acts as a standard diagonal mirror, reflecting a small portion of the incoming light at 90 degrees into the eyepiece. The trapezoidal prism shape refracts the remainder of the light gathered by the telescope's objective away at an angle. The Herschel wedge reflects about 4.6% of the light that passes through one of the prism faces that is flat to 1/10 of the wavelength of the light. The remaining ~95.4% of the light and heat goes into the prism and exits through the other face and out the back door of the housing; thus, the excess light and heat is disposed of and not used for observing. While they decrease the intensity of the light, they do not affect the visible spectra, resulting in a more accurate spectral profile, which can be filtered to bring out certain details. They are an alternative to white light filters, which, despite their name, inherently must block certain visible spectra. + + +== Limitations == +Hershel Wedges present a unique set of hazards and design considerations for the amateur astronomer. Unlike a full aperture ND solar filter, a sub aperture solar filter like a Herschel Wedge allows the full intensity of sunlight to be concentrated by the primary optic. +Secondary optics such as field flatteners, focal reducers, secondary mirrors, and bandpass filters, that are upstream of the Herschel wedge but downstream of the primary optic can overheat and be damaged. Reflectors are extremely dangerous to use with Herschel wedges, since their optical path is poorly contained. While many fear damaging their telescope is the primary reason for avoiding sub-aperture solar filters on reflective telescopes, blinding hazards with reflectors is perhaps even more compelling. +Unlike refractors, whose focal planes lie to the rear of the telescope, reflectors like SCT, Newtonian, RCT, Gregorian, and RASA telescopes have primary mirrors that focus light to a plane in front of the telescope. While some designs use this focal plane as is, others use additional lenses or reflective optics to both correct and move a small portion of this focal plane to a separate area on the telescope. However, it’s important to remember the majority of this focal plane remains in free space, and when it is allowed to focus unfiltered sunlight, like in the case of a Herschel Wedge telescope, it can have disastrous consequences. Looking down the front of a reflecting telescope in direct unfiltered sunlight is no different than staring into the eyepiece of a telescope aimed at the sun without a filter. The large size of reflecting primary mirrors creates the potential for this focal point to burn the inside of a telescope tube or even nearby objects in the vicinity of the telescope. +People who have made a habit of inspecting the inside of their telescope by viewing it from the front or even those who simply want to cap it while its outside may not realize that the same action during the day under sunlight will blind them. Others who use Newtonian telescopes, where a user needs to stand directly above a telescope to enjoy the eyepiece may be burned or blinded by sunlight when slewing on it in the sky. + +It is also important to note that even at 4.5%, (~N.D. 1.35) the light from the sun is still strong enough to burn the retina, and so an appropriate neutral density filter must still be used. + + +== See also == +List of telescope parts and construction + + +== External links == \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/High_Accuracy_Radial_Velocity_Planet_Searcher-0.md b/data/en.wikipedia.org/wiki/High_Accuracy_Radial_Velocity_Planet_Searcher-0.md new file mode 100644 index 000000000..0c1e753f2 --- /dev/null +++ b/data/en.wikipedia.org/wiki/High_Accuracy_Radial_Velocity_Planet_Searcher-0.md @@ -0,0 +1,60 @@ +--- +title: "High Accuracy Radial Velocity Planet Searcher" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/High_Accuracy_Radial_Velocity_Planet_Searcher" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:41:00.058373+00:00" +instance: "kb-cron" +--- + +The High Accuracy Radial Velocity Planet Searcher (HARPS) is a high-precision echelle planet-finding spectrograph installed in 2002 on the ESO's 3.6m telescope at La Silla Observatory in Chile. The first light was achieved in February 2003. HARPS has discovered over 130 exoplanets to date, with the first one in 2004, making it the most successful planet finder behind the Kepler space telescope. It is a second-generation radial-velocity spectrograph, based on experience with the ELODIE and CORALIE instruments. + + +== Characteristics == +The HARPS can attain a precision of 0.97 m/s (3.5 km/h), making it one of only two instruments worldwide with such accuracy. This is due to a design in which the target star and a reference spectrum from a thorium lamp are observed simultaneously using two identical optic fibre feeds, and to careful attention to mechanical stability: the instrument sits in a vacuum vessel which is temperature-controlled to within 0.01 kelvins. The precision and sensitivity of the instrument is such that it incidentally produced the best available measurement of the thorium spectrum. Planet-detection is in some cases limited by the seismic pulsations of the star observed rather than by limitations of the instrument. +The principal investigator on the HARPS is Michel Mayor who, along with Didier Queloz and Stéphane Udry, have used the instrument to characterize the Gliese 581 planetary system, home to one of the smallest known exoplanets orbiting a normal star, and two super-Earths whose orbits lie in the star's habitable zone. +It was initially used for a survey of one-thousand stars. +Since October 2012 the HARPS spectrograph has the precision to detect a new category of planets: habitable super-Earths. This sensitivity was expected from simulations of stellar intrinsic signals, and actual observations of planetary systems. Currently, the HARPS can detect habitable super-Earth only around low-mass stars as these are more affected by gravitational tug from planets and have habitable zones close to the host star. + + +== Discoveries == +This is an incomplete list of exoplanets discovered by the HARPS. The list is sorted by the date of the discovery's announcement. As of December 2017, the list contains 134 exoplanets. + + +== Gallery == + + +== See also == + +Similar instruments: + +HARPS-N is a copy of this instrument installed in the northern hemisphere in 2012. +HARPS3 is an updated design of this instrument that will be installed on an upgraded and roboticised Isaac Newton Telescope, in 2024. +Fiber-optic Improved Next-generation Doppler Search for Exo-Earths, operating at Lick observatory since 2009 +Anglo-Australian Planet Search or AAPS is another southern hemisphere planet search program. +ESPRESSO is a new-generation spectrograph for ESO's VLT. +Automated Planet Finder, at the Lick observatory, commissioned in 2013. +CAFE (Calar Alto Fibre-fed Echelle spectrograph) installed on the Calar Alto Observatory's 2.2-metre telescope in 2014, and the CARMENES mounted on the 3.5-metre telescope in 2016. +EXPRES is a third generation radial velocity spectrograph that is planned to be installed on the Lowell Discovery Telescope. +Space based detectors : + +CoRoT, spacecraft operating since 2007 +Kepler space telescope, operational until 2018 +Terrestrial Planet Finder, cancelled +Space Interferometry Mission, construction halted in 2010 +Darwin, early studies for a multi-satellite mission + + +== Notes == + + +== References == + + +== External links == + Media related to HARPS spectrograph at Wikimedia Commons +"HARPS Home Page". ESO. Retrieved 25 April 2009. +"The Exoplanet Hunter HARPS: unequalled accuracy and perspectives towards 1 cm/s precision" (PDF). ESO. (Contains list of discoveries from 2005 survey.) +"New Planet-Hunting Technology Accelerates Discovery of Exo-Planets & Solar Systems". Daily Galaxy. 17 June 2008. Archived from the original on 7 October 2008. Retrieved 19 October 2008. +"Astronomers discover 4 new planets". NASA. 27 March 2007. Archived from the original on 22 April 2007. \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Instrument_of_the_Primum_Mobile-0.md b/data/en.wikipedia.org/wiki/Instrument_of_the_Primum_Mobile-0.md new file mode 100644 index 000000000..9240bd962 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Instrument_of_the_Primum_Mobile-0.md @@ -0,0 +1,22 @@ +--- +title: "Instrument of the Primum Mobile" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Instrument_of_the_Primum_Mobile" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:41:02.264020+00:00" +instance: "kb-cron" +--- + +The Instrument of the Primum Mobile is also called the quadrant of Petrus Apianus, because he invented it and described it in the treatise Instrumentum primi mobilis (Nuremberg, 1524). The instrument is used to find sines and cosines. It bears the initials "F.E.D.P.F." [Frater Egnatius Dantis Predicatorum Fecit]. Ignazio Danti dedicated it to Cosimo I de' Medici, as attested by the Medici coat of arms engraved on the front. The instrument was depicted on the ceiling of the Stanzino delle Matematiche in the Uffizi Gallery. + + +== Bibliography == +Mara Miniati, ed. (1991). Museo di storia della scienza: catalogo. Firenze: Giunti. p. 44, board n. 28. ISBN 88-09-20036-5. + + +== References == + + +== External links == +"Museo Galileo - object description". \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Integral_field_spectrograph-0.md b/data/en.wikipedia.org/wiki/Integral_field_spectrograph-0.md new file mode 100644 index 000000000..18b7c75dd --- /dev/null +++ b/data/en.wikipedia.org/wiki/Integral_field_spectrograph-0.md @@ -0,0 +1,30 @@ +--- +title: "Integral field spectrograph" +chunk: 1/3 +source: "https://en.wikipedia.org/wiki/Integral_field_spectrograph" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:41:04.054416+00:00" +instance: "kb-cron" +--- + +Integral field spectrographs (IFS) combine spectrographic and imaging capabilities in the optical or infrared wavelength domains (0.32 μm – 24 μm) to get from a single exposure spatially resolved spectra in a bi-dimensional region. The name originates from the fact that the measurements result from integrating the light on multiple sub-regions of the field. Developed at first for the study of astronomical objects, this technique is now also used in many other fields, such as bio-medical science and Earth remote sensing. Integral field spectrography is part of the broader category of snapshot hyperspectral imaging techniques, itself a part of hyperspectral imaging. + +== Rationale == + +With the notable exception of individual stars, most astronomical objects are spatially resolved by large telescopes. For spectroscopic studies, the optimum would then be to get a spectrum for each spatial pixel in the instrument field of view, getting full information on each target. This is loosely called a datacube from its two spatial and one spectral dimensions. +Since both visible charge-coupled devices (CCD) and infrared detector arrays (staring arrays) used for astronomical instruments are bi-dimensional only, it is a non-trivial feat to develop spectrographic systems able to deliver 3D data cubes from the output of 2D detectors. Such instruments are usually christened 3D spectrographs in the astronomical field and hyperspectral imagers in the non-astronomical ones. +Hyperspectral imagers can be broadly classified in two groups, scanning and non-scanning. The first contains the instruments that build the datacube by combining multiple exposures, scanning along a space axis, a wavelength axis or diagonally through it. Examples include push broom scanning systems, scanning Fabry-Perot and Fourier transform spectrometers. The second group includes the techniques that acquire the whole datacube in a single shot, snapshot imaging spectrometers. Integral field spectrography (IFS) techniques were the first snapshot hyperspectral imaging techniques to be developed. Since then, other snapshot hyperspectral imaging techniques, based for example on tomographic reconstruction or compressed sensing using a coded aperture, have been developed. +One major advantage of the snapshot approach for ground-based telescopic observations is that it automatically provides homogenous data sets despite the unavoidable variability of Earth’s atmospheric transmission, spectral emission and image blurring during exposures. This is not the case for scanned systems for which the data cubes are built by a set of successive exposures. IFS, whether ground or space based, have also the huge advantage to detect much fainter objects in a given exposure than scanning systems, if at the cost of a much smaller sky field area. +After a slow start from the late 1980s on, Integral field spectroscopy has become a mainstream astrophysical tool in the optical to mid-infrared regions, addressing a whole gamut of astronomical sources, essentially any smallish individual object from Solar System asteroids to vastly distant galaxies. + +== Methods == + +Integral field spectrographs use so-called Integral Field Units (IFUs) to reformat incoming light from a small field of view, typically rectangular or hexagonal, into a more suitable shape. This reformatted image can then be spectrally dispersed onto a detector by a diffraction grating, such that none of the spectra of each spatial element overlap. There are currently three different IFU flavors, using respectively a lenslet array, a fiber array or a mirror array. + +=== Lenslet array === + +An enlarged sky image feeds a mini-lens array, typically a few thousand identical lenses each about 1 mm in diameter. The lenslet array output is a regular grid of as many small telescope mirror images, which serves as the input for a multi-slit spectrograph that delivers the data cubes. This approach was advocated in the early 1980s, with the first ever IFS observations in 1987 with the lenslet-based optical TIGER . +Pros are 100% on-sky spatial filling when using a square or hexagonal lenslet shape, high throughput, accurate photometry and an easy to build IFU. A significant con is the suboptimal use of precious detector pixels (~ 50% loss at least) in order to avoid contamination between adjacent spectra. +In 2009 the BIGRE lenslet array was proposed to correctly approach the case of spatial and spectral samplings above the Nyquist rate over diffraction limited scenes, as required by high-contrast imaging spectroscopy. This optical concept widely improves the use of detector pixels thanks to the resulting spectrograph line spread function, minimizing inter-spectra crosstalk effects. +Instruments like the Spectrographic Areal Unit for Research on Optical Nebulae (SAURON) on the William Herschel Telescope and the Spectro-Polarimetric High-Contrast Exoplanet Research (SPHERE) IFS subsystem on European Southern Observatory (ESO)'s Very Large Telescope (VLT) use this technique, in the TIGER and BIGRE version respectively. \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Integral_field_spectrograph-1.md b/data/en.wikipedia.org/wiki/Integral_field_spectrograph-1.md new file mode 100644 index 000000000..fb67701c1 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Integral_field_spectrograph-1.md @@ -0,0 +1,29 @@ +--- +title: "Integral field spectrograph" +chunk: 2/3 +source: "https://en.wikipedia.org/wiki/Integral_field_spectrograph" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:41:04.054416+00:00" +instance: "kb-cron" +--- + +=== Fiber array === +The sky image given by the telescope falls on a fiber-based image slicer. It is typically made of a few thousands fibers each about 0.1 mm diameter, with the square or circular input field reformatted into a narrow rectangular (long-slit-like) output. The image slicer output is then coupled to a classical long-slit spectrograph that delivers the datacubes. A sky demonstrator successfully undertook the first Fiber based IFS observation in 1990. It was followed by the full-fledged SILFID optical instrument some 5 years later. Coupling the circular fibers to a square or hexagonal lenslet array led to better light injection in the fiber and a nearly 100% filling factor of sky light. +Pros are 100% on-sky spatial filling, an efficient use of detector pixels and commercially available fiber-based image slicers. Cons are the sizable light loss in the fibers (~ 25%), their relatively poor photometric accuracy and their inability to work in a cryogenic environment. The latter limits wavelength coverage to less than 1.6 μm. +This technique is used by instruments in many telescopes (such as INTEGRAL at the William Herschel Telescope), and particularly in currently ongoing large surveys of galaxies, such as the Calar Alto Legacy Integral Field Area Survey (CALIFA) at the Calar Alto Observatory, the Sydney-AAO Multi-object Integral-field spectrograph (SAMI) at the Australian Astronomical Observatory, and the Mapping Nearby Galaxies at APO (MaNGA) which is one of the surveys making up the next phase of the Sloan Digital Sky Survey. + +=== Mirror array === +The sky image given by the telescope falls on a mirror-based "slicer," typically made of approximately 30 rectangular mirrors, 0.1 to 0.2 mm wide. The slicer reformats the input field into a collection of thin, adjacent "slices" resembling slits in a conventional multi-object spectrograph. This output is then fed to a classical long-slit spectrograph, which disperses and collects the incoming light. Such data can be reduced in the same fashion as a conventional multi-slit spectrograph, with post processing steps to recombine all spectra into a "cube" containing both spatial and spectral information. The first mirror-based slicer near-infrared IFS, the Spectrometer for Infrared Faint Field Imaging (SPIFFI) got its first science result in 2003. The key mirror slicer system was quickly substantially improved under the Advanced Imaging Slicer code name. A more recent slicer-based IFS is the Keck Cosmic Web Imager, KCWI, which features a choice of three separate slicers covering varying fields of view. This provides flexibility for observers to determine an optimal trade-off between field of view, spatial sampling, spectral resolution, and sensitivity to faint sources. +Pros are high throughput, 100% on-sky spatial filling, optimal use of detector pixels and the capability to work at cryogenic temperatures. On the other hand, it is difficult and expensive to manufacture and to align, especially when working in the optical domain given the more stringent optical surfaces specifications. + +== Status == +IFS are currently deployed in one flavor or another on many large ground-based telescopes, in the visible or near infrared domains, and on some space telescopes as well, in particular on the James Webb Space Telescope (JWST) in the near and middle infrared domains. As the spatial resolution of telescopes in space (and also of ground-based telescopes through adaptive optics based air turbulence corrections) has much improved in recent decades, the need for IFS facilities has become more and more pressing. Spectral resolution is usually a few thousands and wavelength coverage about one octave (i.e. a factor 2 in wavelength). Note that each IFS requires a finely tuned software package to transform the raw counts data in physical units (light intensity versus wavelength on precise sky locations) + +== Panoramic IFS == + +With each spatial pixel dispersed on say 4096 spectral pixels on a state of the art 4096 x 4096 pixel detector, IFS fields of view are severely limited, ~10 arc second across when fed by an 8–10 m class telescope. That in turn mainly limits IFS-based astrophysical science to single small targets. A much larger field of view, 1 arc minute across, or a sky area 36 times larger, is needed to cover hundreds of highly distant galaxies, in a single, if very long (up to 100 hours), exposure. This in turn requires to develop IFS systems featuring at least about half a billion detector pixels. +The brute force approach would have been to build huge spectrographs feeding gigantic detector arrays. Instead, the two Panoramic IFS in operation by 2022, Multi-unit spectroscopic explorer (MUSE) and Visible Integral-field Replicable Unit Spectrograph (VIRUS), are made of respectively 24 and 120 serial-produced optical IFS. This results in substantially smaller and cheaper instruments. The mirror slicer based MUSE instrument started operation at the VLT in 2014 and the fiber sliced based VIRUS on the Hobby–Eberly Telescope in 2021. + +== Multi-Object IFS == +It is conceptually straightforward to combine the capabilities of Integral Field Spectroscopy and Multi-Object Spectroscopy in a single instrument. This can be done by deploying a number of small IFUs in a large sky patrol field, possibly a degree or more across. In that way, quite detailed information on, for example, a number of selected galaxies can be obtained in one go. There is of course a tradeoff between the spatial coverage on each target and the total number accessible of targets. The Fibre Large Array Multi Element Spectrograph (FLAMES), the first instrument featuring this capability, had first light in this mode at the VLT in 2002. A number of such facilities are now in operation targeting visible and near infrared wavelengths. \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Integral_field_spectrograph-2.md b/data/en.wikipedia.org/wiki/Integral_field_spectrograph-2.md new file mode 100644 index 000000000..d0b403b87 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Integral_field_spectrograph-2.md @@ -0,0 +1,25 @@ +--- +title: "Integral field spectrograph" +chunk: 3/3 +source: "https://en.wikipedia.org/wiki/Integral_field_spectrograph" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:41:04.054416+00:00" +instance: "kb-cron" +--- + +One such approach was used by the SDSS MaNGA program, Mapping Nearby Galaxies at Apache Point Observatory. MaNGA used IFUs composed of hexagonal fiber bundles to survey about ~10,000 nearby galaxies around redshift 0.03, studying their dynamical state, composition, and formation history. MaNGA was able to use 17 IFU fiber bundles per spectroscopic plate, efficiently targeting many objects simultaneously. +A clever alternative approach to obtaining spatially resolved spectroscopy of many objects simultaneously is the MSA-3D program which uses the micro-shutter array of the JWST NIRSpec instrument to target many objects simultaneously. While not strictly an integral-field unit, the MSA-3D program takes many exposures while "stepping" the conventional slitmask provided by the MSA across the sky. These exposures can be combined after the fact to provide full, 3D spatial and spectral information on each object. While the MSA-3D approach provides much lower spatial resolution than the IFU provided with NIRSpec, and requires many more exposures, it has the advantage of being able to target dozens of nearby objects simultaneously. +Even larger latitude in the choice of coverage of the patrol field has been proposed under the name of Diverse Field Spectroscopy (DFS) which would allow the observer to select arbitrary combinations of sky regions to maximize observing efficiency and scientific return. This requires technological developments, in particular versatile robotic target pickups and photonic switchyards. + +== Three-dimensional detectors == +Other techniques can achieve the same ends at different wavelengths. In particular, at radio wavelengths, simultaneous spectral information is obtained with heterodyne receivers, featuring large frequency coverage and huge spectral resolution. +In the X-ray domain, owing to the high energy of individual photons, aptly called 3D photon counting detectors not only measure on the fly the 2D position of incoming photons but also their energy, hence their wavelength. Note nevertheless that spectral information is very coarse, with spectral resolutions ~10 only. One example is the Advanced CCD Imaging Spectrometer (ACIS) on NASA’s Chandra X-ray Observatory. +In the Visible-Near Infrared, this approach is a lot harder with the much less energetic photons. Nevertheless small format superconducting detectors, with limited spectral resolution ~ 30 and cooled below 0.1 K, have been developed and successfully used, such as for example the 32x32 pixels Array Camera for Optical to Near-infrared Spectrophotometry (ARCONS) Camera at the Hale 200” Telescope. In contrast, ‘classical’ IFS usually feature spectral resolutions of a few thousands. + +== References == + +== External links == +Optical 3D spectroscopy for Astronomy by Roland Bacon and Guy Monnet, ISBN 978-3-527-41202-0 +The Integral Field Spectroscopy wiki +Integral field spectroscopy — A brief introduction by Jeremy Allington-Smith of the Durham Astronomical Instrumentation Group \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/International_Coronelli_Society_for_the_Study_of_Globes-0.md b/data/en.wikipedia.org/wiki/International_Coronelli_Society_for_the_Study_of_Globes-0.md index cca57dabf..c4b2d21e0 100644 --- a/data/en.wikipedia.org/wiki/International_Coronelli_Society_for_the_Study_of_Globes-0.md +++ b/data/en.wikipedia.org/wiki/International_Coronelli_Society_for_the_Study_of_Globes-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/International_Coronelli_Society_for_the_Study_of_Globes" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:37:12.099450+00:00" +date_saved: "2026-05-05T09:41:05.273040+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/International_Pulsar_Timing_Array-0.md b/data/en.wikipedia.org/wiki/International_Pulsar_Timing_Array-0.md new file mode 100644 index 000000000..2686dd836 --- /dev/null +++ b/data/en.wikipedia.org/wiki/International_Pulsar_Timing_Array-0.md @@ -0,0 +1,36 @@ +--- +title: "International Pulsar Timing Array" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/International_Pulsar_Timing_Array" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:41:06.414535+00:00" +instance: "kb-cron" +--- + +The International Pulsar Timing Array (IPTA) is a multi-institutional, multi-telescope collaboration of pulsar timing arrays (PTAs). It comprises the European Pulsar Timing Array (EPTA), the North American Nanohertz Observatory for Gravitational Waves (NANOGrav), the Parkes Pulsar Timing Array (PPTA) in Australia, the Indian Pulsar Timing Array Project (InPTA), the Chinese Pulsar Timing Array (CPTA), the Meerkat Pulsar Timing Array (MPTA), and African Pulsar Timing (APT). The goal of the IPTA is to detect ultra-low-frequency gravitational waves, such as from mergers of supermassive black holes, using an array of over 100 pulsars. + + +== Overview == +The experiment exploits the predictability of the times of arrival (TOAs) of pulses from millisecond pulsars (MSPs) and uses them as a system of galactic clocks. Disturbances in the clocks will be measurable at the Earth. A disturbance from a gravitational wave background will have a particular signature across the ensemble of pulsars called the Hellings & Downs correlation for which multiple PTAs have strong evidence. +The experiment is analogous to ground-based interferometric detectors such as LIGO and VIRGO, where the time of flight of a laser beam is measured along a particular path and compared to the time of flight along an orthogonally oriented path. Instead of the time of flight of a laser beam, the IPTA is measuring the time of flight of an electromagnetic pulse from the pulsar. Instead of 4 km arms, as in the case of LIGO, the 'arms' of the IPTA are thousands of light-years - the distance between the pulsars and the Earth. +These differences between the IPTA and the ground-based interferometers allow them to probe a completely different range of gravitational-wave frequencies and thus a different sources. Whereas ground-based detectors are sensitive to between tens and thousands of Hz, the IPTA is sensitive to between tens and hundreds of nanohertz. The primary source of gravitational waves in this range is expected to be binary mergers of supermassive black holes with billions of solar masses, thought to be abundant in the universe at the centers of galaxies, resulting from previous mergers of those galaxies. +The resources of the IPTA are substantial. The EPTA uses large quantities of time on Europe's five 100-meter class telescopes: the Lovell Telescope in England, the Effelsberg 100-m Radio Telescope in Germany, the Sardinia Radio Telescope in Italy, the Westerbork Synthesis Radio Telescope in the Netherlands, and the Nançay Radio Telescope in France. Together these five telescopes make up the Large European Array for Pulsars (LEAP), in which they operate together as a single 300-meter class telescope. NANOGrav uses about 1 day per month of time at the 100 m Green Bank Telescope, and prior to its collapse, 0.5 days per month at the 300 m Arecibo Observatory in Puerto Rico. The PPTA uses several days per month at the 64 m Parkes Radio Telescope in Australia. +Pulsar timing was tied for top ranking in the "medium size" category for priorities from the Particle Astrophysics and Gravitational Panel of the Astro2010 Decadal Review sponsored by the U.S. National Academy of Sciences. +The IPTA is coordinated and advised by the IPTA Steering Committee, a seven-member committee with two representatives from each of the three IPTA consortium members plus the immediate past chair. Currently on the committee are Richard Manchester (current chair; CSIRO Astronomy and Space Science; PPTA), Willem van Straten (Swinburne University of Technology; PPTA), Scott Ransom (National Radio Astronomy Observatory; NANOGrav), Ingrid Stairs (University of British Columbia; NANOGrav), Ben Stappers (Jodrell Bank Centre for Astrophysics; EPTA), Gilles Theureau (University of Orléans; EPTA), and Andrea Lommen (past chair; Franklin & Marshall College). Each of the three consortium members are also members of the Gravitational Wave International Committee, an advisory council consisting of the leaders of gravitational wave experiments worldwide. + + +== Data release == +The first IPTA data release was on the 12 February 2016, which provided a 2-sigma limit on the amplitude of the Gravitational Wave Background. +The second data release, on 10 September 2019, resulted in the detection of the expected red noise background but not of any supermassive black hole mergers. + + +== References == + + +== External links == +International Pulsar Timing Array +NANOGrav +Parkes Pulsar Timing Array +European Pulsar Timing Array +Indian Pulsar Timing Array \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Jovilabe-0.md b/data/en.wikipedia.org/wiki/Jovilabe-0.md new file mode 100644 index 000000000..ec24711ec --- /dev/null +++ b/data/en.wikipedia.org/wiki/Jovilabe-0.md @@ -0,0 +1,29 @@ +--- +title: "Jovilabe" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Jovilabe" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:41:07.586339+00:00" +instance: "kb-cron" +--- + +The jovilabe is a brass scientific instrument, undated and of unknown maker, currently in the collection of the Museo Galileo in Florence, Italy. +The jovilabe was used by Galileo Galilei to determine the orbital periods of Jupiter's moons and to compute the times of their eclipses. +The instrument is engraved with tables showing the mean motions of each of the four moons. Two connected disks of different diameters are rotated by means of a movable rod. They are used to create a "view from the Sun" of the movements of Jupiter's moons observed from the Earth (movements that seem irregular because of the heliocentric motions of the Earth and Jupiter). +After announcing the discovery of Jupiter's moons in his 1610 treatise Sidereus Nuncius, Galileo began the systematic study of their periods in 1611, developing a micrometer for the purpose. +Galileo immediately realized that eclipses of the moons could provide a precise method to determine longitude. +Galileo compiled tables of the periods that he offered, with his telescopes, first to the King of Spain (1611, 1612, 1616, and 1627-1628), then to the States General of Holland (1637-1641). To convince his Spanish interlocutors that Jupiter and its moons could be observed on unstable ground, such as a ship's deck, Galileo designed a special helmet carrying a small telescope on a hinged mount. The device was named the celatone (celata = "helmet" in Italian). In this second proposal, he also described the advantages of applying the pendulum to the clock. Despite the interest they aroused, neither of his proposals were accepted. + + +== References == + + +== Bibliography == +Mara Miniati, ed. (1991). Museo di storia della scienza: catalogo. Firenze: Giunti. p. 60, board n. 3. ISBN 88-09-20036-5. +Righini Bonelli, Maria Luisa (1971). "Galileo, l'orologio, il giovilabio". Physis Riv. Internaz. Storia Sci. 13 (4): 412–420. +Bedini, Silvio A (1986). "The Galilean jovilabe". Nuncius. 1 (1): 24–26. + + +== External links == +"Museo Galileo - object description". \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Large_Latin_American_Millimeter_Array-0.md b/data/en.wikipedia.org/wiki/Large_Latin_American_Millimeter_Array-0.md new file mode 100644 index 000000000..57897ad28 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Large_Latin_American_Millimeter_Array-0.md @@ -0,0 +1,46 @@ +--- +title: "Large Latin American Millimeter Array" +chunk: 1/2 +source: "https://en.wikipedia.org/wiki/Large_Latin_American_Millimeter_Array" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:41:08.739089+00:00" +instance: "kb-cron" +--- + +The Large Latin American Millimeter Array (LLAMA) is a single-dish 12 m Nasmyth optics antenna which is under construction in the Puna de Atacama desert in the Province of Salta, Argentina, next to the Qubic experiment. The primary mirror accuracy will allow observation from 40 GHz up to 900 GHz. After installation it will be able to join other similar instruments to perform Very Large Base Line Interferometry or to work in standalone mode. Financial support is provided by the Argentinian and Brazilian governments. The total cost of construction, around US$20 million, and operation as well as the telescope time use will be shared equally by the two countries. Construction planning started in July 2014 after the formal signature of an agreement between the main institutions involved. + +== Overview == +LLAMA is a joint project between Argentinian and Brazilian Astronomers to build and operate a radio telescope at submillimeter wavelengths, that can work in stand alone mode or join a Very Long Baseline Interferometry (VLBI) network. The main scientific institutions involved in the project are the Argentine Institute of Radio Astronomy (IAR), and the Núcleo para o Apoio da Rádio Astronomia (NARA), from the Universidade de São Paulo (Brazil). The telescope is located at a very high altitude (4,825 m) where the atmospheric absorption (mostly due to water vapor) allows the observation at the very short wavelengths of less than 1 mm. It is a multipurpose instrument that will have cryogenic receivers with very high sensitivity in order to observe very faint sources, and filters to observe the Sun. + +== History == +The history of the instrument can be traced back to 2007, during the XII Latin American Regional IAU Meeting (LARIM) held in Isla de Margarita (Venezuela). Argentinian radio astronomers discussed the idea with colleagues from South America. The search for the best place for a submillimeter (wavelength less than 1 mm) telescope had started in Argentina in 2003, with a 210 GHz tipper which was installed in different places to investigate the atmospheric opacity. During the XXVII General Assembly in Rio de Janeiro, the project gained a name in a document authored by the leading scientists of the project. In the same document, scientists also proposed the initial science, budget, strategies for construction, site, and other matters. The formal presentation before the Argentinian Science Ministry (MinCyT) was in 2010, while a meeting held at the offices of FAPESP in August 2011 was the kickoff in Brazil. In 2011, MinCyT ranked LLAMA as its astronomical project and in 2012, FAPESP approved a €7 M grant. The final agreement, between MinCyT, FAPESP and Universidade de São Paulo (USP), was signed in June 2014, and on July 9, it was formally presented to the public. +Measurements of the electrical characteristics of the site were carried out in late 2016, and construction of the road to the summit began in December 2016. Assembly of the antenna is planned to take place in 2022, with testing beginning in 2023. + +== Origin of the name == + +The observatory acronym comes from the Quechuan word llama that designates the South American camelid that lives in the region where the telescope is being installed. There is some confusion with the word array, since LLAMA will consist of a single dish antenna, but the instrument will have VLBI technology and can therefore be part of an antenna array with telescopes of other observatories. Moreover, the LLAMA observatory can be expanded in the future by installing other antennas in different sites. +In different official documents the acronym LLAMA may be found expanded as Long Latin American Millimeter Array rather than Large. It is also possible to read Millimetric instead of Millimeter. After some debate, the LLAMA Executive Committee stated that Large Latin American Millimeter Array is the right expansion for the LLAMA acronym. +The observatory logo has as symbols the Southern Cross (upper right), a telescope sketch (bottom right), the acronym (upper left) and a llama profile (bottom left). Although it changed with time, these symbols are present since the beginning. The image illustrating this page is the official logo since August 2014. + +== Science == +LLAMA is a multipurpose instrument, with the capacity to both observe bright sources like the Sun, and very weak sources very far from Earth. The following is a list of different subjects that will be addressed with LLAMA observations. + +=== The Sun === +In the unperturbed solar atmosphere, the shorter the wavelength the deeper the observation. Frequencies near the submillimeter range are produced in the lower chromosphere or the photosphere. Therefore, LLAMA observations will bring new information about the structure of the lower Solar Atmosphere, the active and quiescent filaments and the dynamics of the chromosphere and its magnetic field. The possibility to observe Solar Flares at high frequencies with a high sensitive instrument will give clues about the acceleration of the high energetic particles in the Sun, complementing results obtained with the Solar Submillimeter Telescope. In particular the still unexplained spectral inversion above ≈ 100 GHz. A possible experiment would be to make VLBI solar observations. For example, in a joint observation between LLAMA and some of the ALMA antennas, a spatial resolution of 0.001" would be achieved for λ ≈ 1 mm, corresponding to a distance of 700 m on the solar surface. + +=== Planets === +Extra-solar planetary systems around stars near the Sun. +Proto-planetary disks in star located in the Solar neighborhood. +Near-Earth objects. + +=== Stellar objects === +Star forming regions, young stellar objects, and mechanisms of the star formation. +Non-thermal processes in stellar magnetospheres. +Interaction of stars and remnants of supernova with the interstellar medium. + +=== Astrophysical jets and maser emission === +Astrophysical jets. +Maser phenomena of the recombination lines of the hydrogen atom. +Maser emission in star-forming regions. +Maser emission in late stars stellar envelopes. \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Large_Latin_American_Millimeter_Array-1.md b/data/en.wikipedia.org/wiki/Large_Latin_American_Millimeter_Array-1.md new file mode 100644 index 000000000..bb6c9db41 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Large_Latin_American_Millimeter_Array-1.md @@ -0,0 +1,47 @@ +--- +title: "Large Latin American Millimeter Array" +chunk: 2/2 +source: "https://en.wikipedia.org/wiki/Large_Latin_American_Millimeter_Array" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:41:08.739089+00:00" +instance: "kb-cron" +--- + +=== Galactic and Intergalactic interstellar medium === +Continuum radiation from extragalactic cold dust. +Molecular material in the direction of different stellar objects. +Intergalactic Medium using the detection of molecular absorption lines in the direction of quasars. +Cosmic background radiation. + +=== Galaxies === +Search for CO in galaxies with high redshift. +Molecular abundance. +Active Galactic Nuclei (AGN). +Variation of the fundamental constants by the observation of gravitational lensing. +High redshifts of regions with very high rate of star formation. +Proto-clusters of galaxies. +Space-time distortion produced by massive black holes. + +=== High energies === + +== Optics, Receivers == +The Nasmyth optics will allow the installation of up to as six different heterodyne receivers. There is a consensus for these receivers to use the same spectral bands as ALMA. With this scheme the Nasmyth cabins will allocate receivers for the bands + +It is intended to install a bolometer multi-wavelength camera at the Cassegrain focus, or possibly a camera plus a small heterodyne array. + +== See also == + +Atacama Large Millimeter Array, the biggest millimeter array ever built. +Atacama Pathfinder Experiment (APEX), single dish sub-millimetre telescope built on a modified ALMA prototype antenna +Atacama Submillimeter Telescope Experiment +CARMA a sensitive millimetre-wave array operated by a consortium including Caltech, University of California Berkeley, University of Illinois, University of Maryland and University of Chicago +Cosmic Background Imager a 13 element interferometer operating in Llano de Chajnantor since 1999. +IRAM 30 Meter Telescope (Pico Veleta, Spain), the largest millimetric telescope in the world, operated by IRAM +James Clerk Maxwell Telescope The most sensitive existing sub-millimetre telescope +Plateau de Bure Interferometer, one of the most successful existing millimetre-wave arrays, operated by IRAM +Solar Submillimeter Telescope, the unique solar dedicated submillimeter instrument +List of radio telescopes +List of observatories + +== References == \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/List_of_astronomical_instruments-0.md b/data/en.wikipedia.org/wiki/List_of_astronomical_instruments-0.md index d0fedd3d0..92b72f3dc 100644 --- a/data/en.wikipedia.org/wiki/List_of_astronomical_instruments-0.md +++ b/data/en.wikipedia.org/wiki/List_of_astronomical_instruments-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/List_of_astronomical_instruments" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:36:28.781458+00:00" +date_saved: "2026-05-05T09:39:54.131182+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Lunar_Surface_Electromagnetics_Experiment-0.md b/data/en.wikipedia.org/wiki/Lunar_Surface_Electromagnetics_Experiment-0.md new file mode 100644 index 000000000..e3ce8ecbe --- /dev/null +++ b/data/en.wikipedia.org/wiki/Lunar_Surface_Electromagnetics_Experiment-0.md @@ -0,0 +1,25 @@ +--- +title: "Lunar Surface Electromagnetics Experiment" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Lunar_Surface_Electromagnetics_Experiment" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:41:09.895647+00:00" +instance: "kb-cron" +--- + +The Lunar Surface Electromagnetics Experiment (LuSEE-Night) is a planned robotic radio telescope observatory designed to land and function on the far side of Earth's Moon. The project is under development by the U.S. Department of Energy Brookhaven National Laboratory, the DOE Office of Science, UC Berkeley’s Space Sciences Laboratory and the National Aeronautics and Space Administration. If successfully deployed and activated, LuSEE-Night will attempt measurements of an early period of the history of the Universe that occurred relatively soon after the Big Bang, referred to as the Dark Ages of the Universe, which predates the formation of luminous stars and galaxies. The instrument is planned to be landed on the lunar far side as soon as 2026 aboard the Blue Ghost Mission 2 lunar lander. LuSEE-Night, not to be confused with a companion lander planned for lunar landing in 2024 named LuSEE-Lite, is to be delivered to the lunar far side by Commercial Lunar Payload Services (CLPS). + + +== See also == +Netherlands–China Low-Frequency Explorer (NCLE) +Chronology of the universe +Large Aperture Experiment to Detect the Dark Ages +Lunar Crater Radio Telescope + + +== References == + + +== External links == +March 2023 NASA LuSEE-Night statement \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Mariner's_astrolabe-0.md b/data/en.wikipedia.org/wiki/Mariner's_astrolabe-0.md index fcad7702f..da25c9218 100644 --- a/data/en.wikipedia.org/wiki/Mariner's_astrolabe-0.md +++ b/data/en.wikipedia.org/wiki/Mariner's_astrolabe-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Mariner's_astrolabe" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:37:19.216761+00:00" +date_saved: "2026-05-05T09:41:11.105505+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Stanford_Dish_(Stanford_Radio_Telescope)-0.md b/data/en.wikipedia.org/wiki/Stanford_Dish_(Stanford_Radio_Telescope)-0.md new file mode 100644 index 000000000..d16a43672 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Stanford_Dish_(Stanford_Radio_Telescope)-0.md @@ -0,0 +1,38 @@ +--- +title: "Stanford Dish (Stanford Radio Telescope)" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Stanford_Dish_(Stanford_Radio_Telescope)" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:40:32.590061+00:00" +instance: "kb-cron" +--- + +The Stanford Dish, known locally as the Dish, is a steerable radio antenna in the Stanford, California foothills. "The Dish" is also used locally to refer to the surrounding hiking area. +The 150-foot-diameter (46 m) Dish was built in 1961 by the Stanford Research Institute (now SRI International). The cost to construct the antenna was $4.5 million, and was funded by the United States Air Force. In the 1960s the Dish was used to provide information on Soviet radar installations by detecting radio signals bounced off the moon. +Later on, the Dish was used to communicate with satellites and spacecraft. With its unique bistatic range radio communications, where the transmitter and receiver are separate units, the powerful radar antenna was well-suited for communicating with spacecraft in regions where conventional radio signals may be disrupted. +At one point, the Dish transmitted signals to each of the Voyager craft that NASA dispatched into the outer reaches of the Solar System. In 1982 it was used to rescue the amateur radio satellite UoSAT-1. + + +== Later uses == +As of 2018, the Dish is still actively used for academic and research purposes. It is owned by the U.S. Government and operated by SRI International. It is used for commanding and calibrating spacecraft and for radio astronomy measurements. + + +== Recreational route == +The area around the Dish offers a popular 3.5 mile recreational trail, visited by an average of 1,500–1,800 people daily. The trail around the dish is known for its rolling hills and beautiful views, which on a clear day extend to San Jose, San Francisco, and the East Bay. The Stanford Running Club hosts an annual Dish Race and fun run that forms a 3.25 mile loop around the Dish trail. +While hikers, walkers, and runners are welcome, bicycles and dogs are not allowed on the trail. It is open during daylight hours: + +As of June 2018, 360 cows were grazing on the grounds of the Stanford Dish. Stanford leases the land to farmers who own the cows. + + +== See also == +Millstone Hill – a similar SRI-built antenna in Massachusetts +Sugar Grove Station – site of a never-completed 1960s SRI project for a 600-foot steerable antenna in West Virginia + + +== References == + + +== External links == +Stanford Dish Area – official web page +SRI Dish page (archived) \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Tinamou_egg-0.md b/data/en.wikipedia.org/wiki/Tinamou_egg-0.md new file mode 100644 index 000000000..3cec733ee --- /dev/null +++ b/data/en.wikipedia.org/wiki/Tinamou_egg-0.md @@ -0,0 +1,14 @@ +--- +title: "Tinamou egg" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Tinamou_egg" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:39:47.762183+00:00" +instance: "kb-cron" +--- + +The tinamou egg in Darwin's collection is an egg from the spotted nothura, and is the only specimen left in Darwin's collections during his HMS Beagle voyage. The egg has a large crack because Darwin put it in a box too small for it. It was rediscovered by volunteer Liz Wetton in February 2009, the 200th year of Darwin's birth, while she was sorting the egg collection in the zoology museum at the University of Cambridge. + + +== References == \ No newline at end of file diff --git a/data/en.wikipedia.org/wiki/Vedic_science-0.md b/data/en.wikipedia.org/wiki/Vedic_science-0.md index a85a18449..d713c1d4b 100644 --- a/data/en.wikipedia.org/wiki/Vedic_science-0.md +++ b/data/en.wikipedia.org/wiki/Vedic_science-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Vedic_science" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:26:31.763019+00:00" +date_saved: "2026-05-05T09:39:48.966221+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Westphal_balance-0.md b/data/en.wikipedia.org/wiki/Westphal_balance-0.md index ba9bc71a5..3db62fd4d 100644 --- a/data/en.wikipedia.org/wiki/Westphal_balance-0.md +++ b/data/en.wikipedia.org/wiki/Westphal_balance-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Westphal_balance" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:38:10.254606+00:00" +date_saved: "2026-05-05T09:39:50.171625+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Yuasa_Phenomenon-0.md b/data/en.wikipedia.org/wiki/Yuasa_Phenomenon-0.md index abab4f9a0..022e07b77 100644 --- a/data/en.wikipedia.org/wiki/Yuasa_Phenomenon-0.md +++ b/data/en.wikipedia.org/wiki/Yuasa_Phenomenon-0.md @@ -4,7 +4,7 @@ chunk: 1/1 source: "https://en.wikipedia.org/wiki/Yuasa_Phenomenon" category: "reference" tags: "science, encyclopedia" -date_saved: "2026-05-05T09:35:46.247050+00:00" +date_saved: "2026-05-05T09:39:51.411882+00:00" instance: "kb-cron" --- diff --git a/data/en.wikipedia.org/wiki/Zurich_Notebook-0.md b/data/en.wikipedia.org/wiki/Zurich_Notebook-0.md new file mode 100644 index 000000000..b7c9e37b1 --- /dev/null +++ b/data/en.wikipedia.org/wiki/Zurich_Notebook-0.md @@ -0,0 +1,14 @@ +--- +title: "Zurich Notebook" +chunk: 1/1 +source: "https://en.wikipedia.org/wiki/Zurich_Notebook" +category: "reference" +tags: "science, encyclopedia" +date_saved: "2026-05-05T09:39:52.569701+00:00" +instance: "kb-cron" +--- + +The Zurich Notebook is one of Albert Einstein's notebooks, from his time in Zürich. It contains much of Einstein's foundational work on general relativity. + + +== References == \ No newline at end of file