Observational Methods
... B. No, you need to know two more variables. C. Yes but one of the variables above is not needed. D. Yes you can using all of the above variables. ...
... B. No, you need to know two more variables. C. Yes but one of the variables above is not needed. D. Yes you can using all of the above variables. ...
The Surveyors` Heliotrope
... them, and to replace them about every four minutes, according to the motion of the sun. . . . They will show a precise luminous point, even though haze, so frequent on the eastern seashore, when the outline of the hill itself, upon which they stand, cannot be traced.” In the course of the ensuing ye ...
... them, and to replace them about every four minutes, according to the motion of the sun. . . . They will show a precise luminous point, even though haze, so frequent on the eastern seashore, when the outline of the hill itself, upon which they stand, cannot be traced.” In the course of the ensuing ye ...
Coast Steel Fabricators
... and other topographical features • Wind speed-up over hills • Prevailing wind speed and direction • Air temperature and density ...
... and other topographical features • Wind speed-up over hills • Prevailing wind speed and direction • Air temperature and density ...
Concepts discussed Jargon and conventions
... | Photometry | Antenna temperature | Photometric calibration | Color index or magnitude difference ...
... | Photometry | Antenna temperature | Photometric calibration | Color index or magnitude difference ...
Ground-Conjugate Wide Field Adaptive Optics for the ELTs F. Rigaut
... Figure 2 displays the natural and compensated median FWHMs at Cerro Pachon and Cerro Paranal for the three bands V, J and K, versus the eld of view. This gure shows that this compensation scheme, like any other phase compensation method, is very wavelength dependant. Apparently, a threshold is pas ...
... Figure 2 displays the natural and compensated median FWHMs at Cerro Pachon and Cerro Paranal for the three bands V, J and K, versus the eld of view. This gure shows that this compensation scheme, like any other phase compensation method, is very wavelength dependant. Apparently, a threshold is pas ...
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 ...
CCD Observatory in school - EU-HOU
... Although a webcam itself is equipped with a lens, this lens is practically useless – apart from observations of meteorites – due to its small aperture and short focal ...
... Although a webcam itself is equipped with a lens, this lens is practically useless – apart from observations of meteorites – due to its small aperture and short focal ...
Atmospheric Turbulence and its Influence on Adaptive Optics
... Adaptive Optics (AO) is still a relatively young branch of astronomical instrumentation. Different technologies are developing all the time and it can be difficult keeping up with all the different acronyms (e.g. GLAO, MOAO, MCAO, SLGS, RLGS, etc..) never mind the technologies themselves. It is easy ...
... Adaptive Optics (AO) is still a relatively young branch of astronomical instrumentation. Different technologies are developing all the time and it can be difficult keeping up with all the different acronyms (e.g. GLAO, MOAO, MCAO, SLGS, RLGS, etc..) never mind the technologies themselves. It is easy ...
Full paper - The Institute of Mathematical Sciences
... medium energy resolution spectral studies and localization of Transients in soft and hard X-ray bands. • A Scanning Sky X-ray Monitor to detect and monitor Transients and known objects. • High time resolution (10 µs ) and high count rate capability ( 40 k Counts with PHA and 60 k Counts without PHA ...
... medium energy resolution spectral studies and localization of Transients in soft and hard X-ray bands. • A Scanning Sky X-ray Monitor to detect and monitor Transients and known objects. • High time resolution (10 µs ) and high count rate capability ( 40 k Counts with PHA and 60 k Counts without PHA ...
A Taxonomy of IRMOS/MOAO Architectures and their Consequences
... MEMS DMs do not have this entire range available, thus a second DM, denoted as a “woofer,” must be used to handle some of the stroke range. These are the basic options for a woofer: 1. Adaptive secondary. The goal of the telescope design is to not preclude eventual mounting of an adaptive secondary ...
... MEMS DMs do not have this entire range available, thus a second DM, denoted as a “woofer,” must be used to handle some of the stroke range. These are the basic options for a woofer: 1. Adaptive secondary. The goal of the telescope design is to not preclude eventual mounting of an adaptive secondary ...
Reflector collimation
... to identify the optical parts just described. This is best done during daylight, with the telescope aimed at the ceiling or the sky (be careful to avoid the Sun). The illustration to the right shows what you should see: the secondary mirror in its holder, its elliptical face tilted 45° and appearing ...
... to identify the optical parts just described. This is best done during daylight, with the telescope aimed at the ceiling or the sky (be careful to avoid the Sun). The illustration to the right shows what you should see: the secondary mirror in its holder, its elliptical face tilted 45° and appearing ...
The WSO, a world-class observatory for the ultraviolet
... subsystem is reduced. Hence, the WSO delivers considerably enhanced effective area. This thoughput is similar to that offered by the Cosmic Origins Spectrograph (COS) at the longer wavelengths, which is to be mounted on HST in 2004, but COS has an inferior spectral resolution (R~24,000 max). With a ...
... subsystem is reduced. Hence, the WSO delivers considerably enhanced effective area. This thoughput is similar to that offered by the Cosmic Origins Spectrograph (COS) at the longer wavelengths, which is to be mounted on HST in 2004, but COS has an inferior spectral resolution (R~24,000 max). With a ...
Copyright 2003 Society of Photo-Optical Instrumentation Engineers
... The Very Large Telescope Interferometer (VLTI) owned by the European Southern Observatory (ESO) exists in the coherent combination of four VLT Unit Telescopes and of several moveable 1.8m Auxiliary Telescopes. A key technique for optical aperture synthesis (interferometric) instruments is the co-pha ...
... The Very Large Telescope Interferometer (VLTI) owned by the European Southern Observatory (ESO) exists in the coherent combination of four VLT Unit Telescopes and of several moveable 1.8m Auxiliary Telescopes. A key technique for optical aperture synthesis (interferometric) instruments is the co-pha ...
Ay 105 Lab Experiment #2: Geometric optics
... Part A Measurements. Experiment with how to read the test target patterns by having one member of your group move the blocking source around in front of the lamp. Once you are comfortable, use the micrometer eyepiece to measure the sizes of an element (one “line pair”) in each group that is visible, ...
... Part A Measurements. Experiment with how to read the test target patterns by having one member of your group move the blocking source around in front of the lamp. Once you are comfortable, use the micrometer eyepiece to measure the sizes of an element (one “line pair”) in each group that is visible, ...
document
... WFE to be budgeted among pri, sec, flat, and tertiary mirrors — detailed breakdown to be determined How sensitive are cost & schedule to our WFE specification? Encircled Energy specification needs to be defined — central obstruction 40% radius, 16% area — with this obstruction alone, EE=50% at 0.088 ...
... WFE to be budgeted among pri, sec, flat, and tertiary mirrors — detailed breakdown to be determined How sensitive are cost & schedule to our WFE specification? Encircled Energy specification needs to be defined — central obstruction 40% radius, 16% area — with this obstruction alone, EE=50% at 0.088 ...
Sodium D-line Splitting
... the diffraction pattern consists of diffraction modulated interference fringes. The quantity (e+b) is called the grating element and N (= 1/ (e+b)) is the number of slits per unit length, which could typically be 300 to 12000 lines per inch. For a large number of slits, the diffraction pattern consi ...
... the diffraction pattern consists of diffraction modulated interference fringes. The quantity (e+b) is called the grating element and N (= 1/ (e+b)) is the number of slits per unit length, which could typically be 300 to 12000 lines per inch. For a large number of slits, the diffraction pattern consi ...
MAESTRO Primary Structure Allowable Deflections
... Rigid Body Motion The rigid body motions defined by the gravity deflections can be used to evaluate boresight changes. Furthermore, rigid body motion of the optical bench relative to the telescope will also occur, which can be approximated by the absolute deflections of the injection optics CG posit ...
... Rigid Body Motion The rigid body motions defined by the gravity deflections can be used to evaluate boresight changes. Furthermore, rigid body motion of the optical bench relative to the telescope will also occur, which can be approximated by the absolute deflections of the injection optics CG posit ...
Florencio Utreras - michael-stanton
... The EVALSO Project • Paranal Observatory is located 130 Km South of Antofagasta in Chile • To instal Optical Fibre from Cerro Paranal to Antofagasta and connect there with REUNA and RedCLARA • Purpose, to develop new modes of observation ...
... The EVALSO Project • Paranal Observatory is located 130 Km South of Antofagasta in Chile • To instal Optical Fibre from Cerro Paranal to Antofagasta and connect there with REUNA and RedCLARA • Purpose, to develop new modes of observation ...
Lifecycle of Dust in Galaxies - The National Academies of Sciences
... physical resolution of ∼10 pc. For the LMC, the global view of the ISM dust properties derived from the SAGE-LMC data is presented by Bernard et al. (2008). Among the results is a derivation of the total mass of the ISM, which appears to be a factor of two larger than currently known from gas measur ...
... physical resolution of ∼10 pc. For the LMC, the global view of the ISM dust properties derived from the SAGE-LMC data is presented by Bernard et al. (2008). Among the results is a derivation of the total mass of the ISM, which appears to be a factor of two larger than currently known from gas measur ...
Very Large Telescope
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The Very Large Telescope (VLT) is a telescope operated by the European Southern Observatory on Cerro Paranal in the Atacama Desert of northern Chile. The VLT consists of four individual telescopes, each with a primary mirror 8.2 m across, which are generally used separately but can be used together to achieve very high angular resolution. The four separate optical telescopes are known as Antu, Kueyen, Melipal and Yepun, which are all words for astronomical objects in the Mapuche language. The telescopes form an array which is complemented by four movable Auxiliary Telescopes (ATs) of 1.8 m aperture.The VLT operates at visible and infrared wavelengths. Each individual telescope can detect objects roughly four billion times fainter than can be detected with the naked eye, and when all the telescopes are combined, the facility can achieve an angular resolution of about 0.001 arc-second (This is equivalent to roughly 2 meters resolution at the distance of the Moon).In single telescope mode of operation angular resolution is about 0.05 arc-second.The VLT is the most productive ground-based facility for astronomy, with only the Hubble Space Telescope generating more scientific papers among facilities operating at visible wavelengths. Among the pioneering observations carried out using the VLT are the first direct image of an exoplanet, the tracking of individual stars moving around the supermassive black hole at the centre of the Milky Way, and observations of the afterglow of the furthest known gamma-ray burst.