Current Status of the Hobby-Eberly Telescope Wide Field
... The reference design is a four-mirror design with two concave 1 m diameter mirrors, one concave 0.9 m diameter mirror, and one convex 0.23 m diameter mirror. Since the corrector is designed for feeding optical fibers at f/3.65 the chief ray from all field angles is normal to the focal surface. This ...
... The reference design is a four-mirror design with two concave 1 m diameter mirrors, one concave 0.9 m diameter mirror, and one convex 0.23 m diameter mirror. Since the corrector is designed for feeding optical fibers at f/3.65 the chief ray from all field angles is normal to the focal surface. This ...
instructions
... can see a large selection at www.ingenious.org.uk including many that are not currently on display in the Museum. Highlights of the collection include replicas of Galileo’s and Newton’s original telescopes. ...
... can see a large selection at www.ingenious.org.uk including many that are not currently on display in the Museum. Highlights of the collection include replicas of Galileo’s and Newton’s original telescopes. ...
template
... • Further consolidation of interface requirements. • Focusing mechanism development (dedicated TDA planned). • Schedule driven by M1 polishing (dedicated TDA planned). SAFARI: • Further consolidation of interface requirements. • Early selection of focal plane detector technology required. • FTS scan ...
... • Further consolidation of interface requirements. • Focusing mechanism development (dedicated TDA planned). • Schedule driven by M1 polishing (dedicated TDA planned). SAFARI: • Further consolidation of interface requirements. • Early selection of focal plane detector technology required. • FTS scan ...
Presentation Title, Arial Regular 29pt Sub title, Arial Regular 24pt
... 6 x 22m dishes (ie. 15 baselines, from 30 m to 6 km) frequency coverage: ≈ 1 100 GHz (3mm to 20cm) dualfrequency & dualpolarisation operation high time resolution dedicated expert staff & international user community (incl. a large number of students) • NOW: bandwidth is 2 ...
... 6 x 22m dishes (ie. 15 baselines, from 30 m to 6 km) frequency coverage: ≈ 1 100 GHz (3mm to 20cm) dualfrequency & dualpolarisation operation high time resolution dedicated expert staff & international user community (incl. a large number of students) • NOW: bandwidth is 2 ...
Light Source Test at the Telescope Array Site
... 20 flights in TA site on Oct. 14, 15, and 16 in last year. We had analyzed the four calibration operation data to the center PMT 77 in camera 07 which the distance between the octocopter and the mirror is about 1.0 km. The standard deviation of the octocopter position for the flights are less than a ...
... 20 flights in TA site on Oct. 14, 15, and 16 in last year. We had analyzed the four calibration operation data to the center PMT 77 in camera 07 which the distance between the octocopter and the mirror is about 1.0 km. The standard deviation of the octocopter position for the flights are less than a ...
Let`s Observe the Andromeda Nebula (M31)!
... In 1920, the Great Debate over this problem was held between two American astronomers: Harlow Shapley and Heber Curtis. ...
... In 1920, the Great Debate over this problem was held between two American astronomers: Harlow Shapley and Heber Curtis. ...
New Meade 60 EQ-D 8-03
... Line up one of the leg braces (4, Fig. 1) between the opening of one of the tripod leg brace supports (5, Fig. 1) on the tripod so that one of the short screws will be able to pass through the holes of the leg brace support and the leg brace. Using a Phillips-head screwdriver, thread one of the shor ...
... Line up one of the leg braces (4, Fig. 1) between the opening of one of the tripod leg brace supports (5, Fig. 1) on the tripod so that one of the short screws will be able to pass through the holes of the leg brace support and the leg brace. Using a Phillips-head screwdriver, thread one of the shor ...
Telescope notes
... • Combines information from several widely spread radio telescopes as if it came from a single dish • Resolution will be that of dish whose diameter = largest separation between dishes ...
... • Combines information from several widely spread radio telescopes as if it came from a single dish • Resolution will be that of dish whose diameter = largest separation between dishes ...
1 Introduction - Arecibo Observatory
... observations at wavelengths between λ6 m and 3 cm (frequencies of 47 MHz to 10 GHz). Over the past few years it has contributed significantly to investigations of solar system bodies via radar imaging, the discovery and subsequent study of new pulsars, the use of binary pulsars as laboratories for g ...
... observations at wavelengths between λ6 m and 3 cm (frequencies of 47 MHz to 10 GHz). Over the past few years it has contributed significantly to investigations of solar system bodies via radar imaging, the discovery and subsequent study of new pulsars, the use of binary pulsars as laboratories for g ...
Laboratory Exercise 7 - School of Physics and Astronomy
... part you will use a diffraction grating to produce the line spectra of a number of elements, and will investigate how close in wavelength two lines can be before they become indistinguishable. This property is called the chromatic resolution of the instrument or sometimes, when there is no possibili ...
... part you will use a diffraction grating to produce the line spectra of a number of elements, and will investigate how close in wavelength two lines can be before they become indistinguishable. This property is called the chromatic resolution of the instrument or sometimes, when there is no possibili ...
60AZ-AR - OPT Telescopes
... nebulas are clouds of gas. The two easiest to see in the Northern Hemisphere are the Orion nebula during the winter and the Triffid nebula during the summer. These are large clouds of gas in which new stars are being born. Some nebulas are the remains of stars exploding. These explosions are called ...
... nebulas are clouds of gas. The two easiest to see in the Northern Hemisphere are the Orion nebula during the winter and the Triffid nebula during the summer. These are large clouds of gas in which new stars are being born. Some nebulas are the remains of stars exploding. These explosions are called ...
*************DST
... telecentric design and a spectral resolution of 250,000. It covers the visible part of the spectrum and can be operated in intensity mode, to record Stokes-I line profiles of 2D images, and in polarization mode, to measure the full polarization state of the light along line profiles (I, Q, U, and V) ...
... telecentric design and a spectral resolution of 250,000. It covers the visible part of the spectrum and can be operated in intensity mode, to record Stokes-I line profiles of 2D images, and in polarization mode, to measure the full polarization state of the light along line profiles (I, Q, U, and V) ...
Precision engineering for astronomy
... and Lord Rosse were able to take advantage of their greater sensitivity and angular resolution to make key discoveries such as Uranus and the first detailed observations of the nebulae that we later came to realize were distant galaxies. In 1895, the world’s largest refractor, the Yerkes Observatory ...
... and Lord Rosse were able to take advantage of their greater sensitivity and angular resolution to make key discoveries such as Uranus and the first detailed observations of the nebulae that we later came to realize were distant galaxies. In 1895, the world’s largest refractor, the Yerkes Observatory ...
bringing it closer - eGFI
... short wavelengths (gamma), and representative telescopes that observe at those wavelengths are given. What follows is then a description of those types of telescopes and how they work. 1. Radio waves - The 100-m Green bank Telescope in Green Bank, West Virginia is used to study millimeter-wavelength ...
... short wavelengths (gamma), and representative telescopes that observe at those wavelengths are given. What follows is then a description of those types of telescopes and how they work. 1. Radio waves - The 100-m Green bank Telescope in Green Bank, West Virginia is used to study millimeter-wavelength ...
ISON network development in 2015
... • ISON network is splitting on 3 segments that may be independent in near future: - KIAM scientific international cooperation; - Roscomsos segment (ASPOS OKP); - industry organizations (JSC Vimpel & ASC) • New segment of ISON network for observations under commercial contracts is arranged as part of ...
... • ISON network is splitting on 3 segments that may be independent in near future: - KIAM scientific international cooperation; - Roscomsos segment (ASPOS OKP); - industry organizations (JSC Vimpel & ASC) • New segment of ISON network for observations under commercial contracts is arranged as part of ...
Comparative h- and m-indices for Fifteen Ground- and Space
... Every effort was made to provide a normalized comparison. The h‐index and m‐index are just two of many measures available for benchmarking scientific productivity. Other methodologies include the g‐index (Egghe 2006) and the hg‐ index (Alonso et al. 2010). The h‐index and m‐index values provided ...
... Every effort was made to provide a normalized comparison. The h‐index and m‐index are just two of many measures available for benchmarking scientific productivity. Other methodologies include the g‐index (Egghe 2006) and the hg‐ index (Alonso et al. 2010). The h‐index and m‐index values provided ...
Seeing
... ESO was created in 1962 and is supported by eleven countries: Belgium, Denmark, Finland, France, Germany, Italy, the Netherlands, Portugal, Sweden, Switzerland and United Kingdom. ESO operates three sites in the Atacama desert region in Chile. The Very Large Telescope (VLT) on Paranal is located on ...
... ESO was created in 1962 and is supported by eleven countries: Belgium, Denmark, Finland, France, Germany, Italy, the Netherlands, Portugal, Sweden, Switzerland and United Kingdom. ESO operates three sites in the Atacama desert region in Chile. The Very Large Telescope (VLT) on Paranal is located on ...
Paper
... properly designed system will perform as well as a telescope with a shorter focal ratio. While there will be some focal ratio degradation when driving the fibers at f/6, if this degradation is characterized and the spectrometer designed to be fed at this reduced focal ratio, there will be no loss re ...
... properly designed system will perform as well as a telescope with a shorter focal ratio. While there will be some focal ratio degradation when driving the fibers at f/6, if this degradation is characterized and the spectrometer designed to be fed at this reduced focal ratio, there will be no loss re ...
Antarctic Infra-Red Telescope with a 40cm primary mirror
... because like the sun, Venus doesn’t set during summer in Antarctica. ...
... because like the sun, Venus doesn’t set during summer in Antarctica. ...
Lecture6_v3 - Lick Observatory
... of 10 m, compared with 5 m for the Palomar Telescope in California. The light gathering power of Keck is larger by a factor of a) 2 ...
... of 10 m, compared with 5 m for the Palomar Telescope in California. The light gathering power of Keck is larger by a factor of a) 2 ...
The 1.5 meter solar telescope GREGOR
... 2007). Swirling motions were recently found in the photosphere and also in the chromosphere. They may be another mechanism to transport energy from the solar surface to higher layers of the solar atmosphere (Wedemeyer-Böhm et al. 2012). The time scales of chromospheric dynamics are short, the magne ...
... 2007). Swirling motions were recently found in the photosphere and also in the chromosphere. They may be another mechanism to transport energy from the solar surface to higher layers of the solar atmosphere (Wedemeyer-Böhm et al. 2012). The time scales of chromospheric dynamics are short, the magne ...
Lovell Telescope
The Lovell Telescope /ˈlʌvəl/ is a radio telescope at Jodrell Bank Observatory, near Goostrey, Cheshire in the north-west of England. When construction was finished in 1957, the telescope was the largest steerable dish radio telescope in the world at 76.2 m (250 ft) in diameter;it is now the third largest, after the Green Bank telescope in West Virginia, USA, and the Effelsberg telescope in Germany.It was originally known as the ""250 ft telescope"" or the Radio Telescope at Jodrell Bank, before becoming the Mark I telescope around 1961 when future telescopes (the Mark II, III, and IV) were being discussed. It was renamed to the Lovell Telescope in 1987 after Sir Bernard Lovell, and became a Grade I listed building in 1988. The telescope forms part of the MERLIN and European VLBI Network arrays of radio telescopes.Both Bernard Lovell and Charles Husband were knighted for their roles in creating the telescope. In September 2006, the telescope won the BBC's online competition to find the UK's greatest ""Unsung Landmark"". 2007 marked the 50th anniversary of the telescope.If the air is clear enough, the Mark I telescope can be seen from high-rise buildings in Manchester such as the Beetham Tower, and from as far away as the Pennines, Winter Hill in Lancashire, Snowdonia, Beeston Castle in Cheshire, and the Peak District. It can also be seen from the Terminal 1 restaurant area and departure lounges of Manchester Airport.