Slide 1
... Test of tracker looking through window • An SMR was measured directly at ~1 m • 1 cm thick window was inserted between the tracker and the SMR • The apparent SMR position was measured with the tracker • This was corrected for the refraction of the window • These tests showed agreement to 20 ppm, wh ...
... Test of tracker looking through window • An SMR was measured directly at ~1 m • 1 cm thick window was inserted between the tracker and the SMR • The apparent SMR position was measured with the tracker • This was corrected for the refraction of the window • These tests showed agreement to 20 ppm, wh ...
3P29.pdf
... German Spanish Astronomical Observatory (CAHA) in Almeria (Spain), with the Fibre Optics Cassegrain Echelle Spectrometer (FOCES) (Pfeiffer et al. 1998). During this observing run, a 2048x2048 pixel 150µ Site#1d15 CCD detector was used. The spectrograph set up was chosen to cover the Hα (6563 Å) and ...
... German Spanish Astronomical Observatory (CAHA) in Almeria (Spain), with the Fibre Optics Cassegrain Echelle Spectrometer (FOCES) (Pfeiffer et al. 1998). During this observing run, a 2048x2048 pixel 150µ Site#1d15 CCD detector was used. The spectrograph set up was chosen to cover the Hα (6563 Å) and ...
Slide 1
... Introducing Spitzer The Spitzer Space Telescope is a cryogenically cooled, infrared observatory in space. Spitzer can study objects ranging from our Solar System to the distant reaches of the Universe. The Universe in the Infrared ...
... Introducing Spitzer The Spitzer Space Telescope is a cryogenically cooled, infrared observatory in space. Spitzer can study objects ranging from our Solar System to the distant reaches of the Universe. The Universe in the Infrared ...
Introduction to Astrophotography
... coma, and sometimes also a visible tail. • Unlike the sun, moon, and planets, comets are typically not bright objects and can be quite challenging to photograph. • Short exposures will not bring out the comet’s surrounding coma or it’s tail. • Long exposures (more than a few seconds) will require a ...
... coma, and sometimes also a visible tail. • Unlike the sun, moon, and planets, comets are typically not bright objects and can be quite challenging to photograph. • Short exposures will not bring out the comet’s surrounding coma or it’s tail. • Long exposures (more than a few seconds) will require a ...
LIGO-M080375-V12 (Abbreviations And Acronyms)
... Hydraulic External Pre-Isolator, an element of the SEI that isolates chambers from seismic activity ...
... Hydraulic External Pre-Isolator, an element of the SEI that isolates chambers from seismic activity ...
COrE+ Optics options
... • Reimaging optics module can be included if required to place cold stop for planar pixels • Gaussian beam telescope configuration with 2 lenses is being investigated currently. • Paraxial lens options already added using ray tracing analysis. • Next step to add real lens – requires optimisation for ...
... • Reimaging optics module can be included if required to place cold stop for planar pixels • Gaussian beam telescope configuration with 2 lenses is being investigated currently. • Paraxial lens options already added using ray tracing analysis. • Next step to add real lens – requires optimisation for ...
Manufacture of 8.4 m off-axis segments
... Most large mirrors have a loose tolerance on focus, equivalent to a tolerance on radius of curvature of 1 mm or more. The GMT segments have a much tighter tolerance on focus because of the need for all seven mirrors to have the same image magnification. The requirement is strictly that the segments ...
... Most large mirrors have a loose tolerance on focus, equivalent to a tolerance on radius of curvature of 1 mm or more. The GMT segments have a much tighter tolerance on focus because of the need for all seven mirrors to have the same image magnification. The requirement is strictly that the segments ...
The World`s Easiest Equatorial Mount Instruction Manual
... When using an equatorial mount, you can move your telescope to these settings and find the star that corresponds to that address. You will need to have a Star Atlas to use the equatorial mount. You can purchase one at just about any bookstore on earth. As well, you will need to be able to identify 2 ...
... When using an equatorial mount, you can move your telescope to these settings and find the star that corresponds to that address. You will need to have a Star Atlas to use the equatorial mount. You can purchase one at just about any bookstore on earth. As well, you will need to be able to identify 2 ...
ppt
... Based on a 1996 Optical Telescope Assembly study, the following requirements were placed on JWST's optics: The mirror should be sensitive to 1-5 microns (0.6-30 extended). It should be diffraction limited to 2 microns. It will have to operate at 30-60 K. It should have an areal density of less than ...
... Based on a 1996 Optical Telescope Assembly study, the following requirements were placed on JWST's optics: The mirror should be sensitive to 1-5 microns (0.6-30 extended). It should be diffraction limited to 2 microns. It will have to operate at 30-60 K. It should have an areal density of less than ...
ch 31, stars
... • A telescope that collects and amplifies radio waves is a radio telescope. • Because radio waves have long wavelengths, a radio telescope must be built with a very large objective, usually some form of dish antenna. • The very large array near Socorro, New Mexico has 27 radio telescopes that detect ...
... • A telescope that collects and amplifies radio waves is a radio telescope. • Because radio waves have long wavelengths, a radio telescope must be built with a very large objective, usually some form of dish antenna. • The very large array near Socorro, New Mexico has 27 radio telescopes that detect ...
1 - EPJ Web of Conferences
... iris shutter (see Fig. 1). The angular resolution of the ASC is approx. 0.1 degree. The whole 180 × 180 deg. field of view (FOV) covers 1750 × 1750 pixel area of the CCD chip (see Fig. 1). The three types of CTA telescopes (LST, MST and SST respectively) are designed with FOV of 5, 8 and 10 angular ...
... iris shutter (see Fig. 1). The angular resolution of the ASC is approx. 0.1 degree. The whole 180 × 180 deg. field of view (FOV) covers 1750 × 1750 pixel area of the CCD chip (see Fig. 1). The three types of CTA telescopes (LST, MST and SST respectively) are designed with FOV of 5, 8 and 10 angular ...
PDF
... The X-ray study of pulsars continued with launch of the ROSAT in 1990 (Trümper 1983). Its large collecting area and high spatial resolution allowed detection of synchrotron nebulae, all with linear size of a few parsecs, around several Galactic radio pulsars, including PSRs B1706−44, B1951+32, and ...
... The X-ray study of pulsars continued with launch of the ROSAT in 1990 (Trümper 1983). Its large collecting area and high spatial resolution allowed detection of synchrotron nebulae, all with linear size of a few parsecs, around several Galactic radio pulsars, including PSRs B1706−44, B1951+32, and ...
a history of the mcmath-pierce solar telescope - NSO
... the past four decades. Only now are plans being formed for a solar telescope to surpass its 1.6-meter aperture. An unusual all-reflecting optical system was chosen for the McM-P. A 2-meter heliostat feeds a beam to an open-air, unobstructed mirror system that produces an image of the Sun that’s roug ...
... the past four decades. Only now are plans being formed for a solar telescope to surpass its 1.6-meter aperture. An unusual all-reflecting optical system was chosen for the McM-P. A 2-meter heliostat feeds a beam to an open-air, unobstructed mirror system that produces an image of the Sun that’s roug ...
PULSE@Parkes science and technology overview
... pulsars whose pulsed emission seems to “switch-off” for long periods of time. When “on” these pulsars are bright and can be seen using short observations. When “off” these pulsars are completely undetectable. Unfortunately, the lack of observing time on existing telescopes implies that the statistic ...
... pulsars whose pulsed emission seems to “switch-off” for long periods of time. When “on” these pulsars are bright and can be seen using short observations. When “off” these pulsars are completely undetectable. Unfortunately, the lack of observing time on existing telescopes implies that the statistic ...
orion® starBlast™ 4.5 EQ
... The EZ Finder II works by projecting a tiny red dot (it’s not a laser beam) onto a lens mounted in the front of the unit. When you look through the EZ Finder II, the red dot will appear to float in space, helping you locate even the faintest of deepsky objects. The red dot is produced by a light-emi ...
... The EZ Finder II works by projecting a tiny red dot (it’s not a laser beam) onto a lens mounted in the front of the unit. When you look through the EZ Finder II, the red dot will appear to float in space, helping you locate even the faintest of deepsky objects. The red dot is produced by a light-emi ...
chromospheric telescope of baikal astrophysical observatory. new light
... components, positive and negative, making them from one material and with radii of curvature that are equal in size but different in sign. The latter is very favorable for the mutual control of radii of curvature and lens surface shape when manufactured. The lens reconstructs and enlarges a solar im ...
... components, positive and negative, making them from one material and with radii of curvature that are equal in size but different in sign. The latter is very favorable for the mutual control of radii of curvature and lens surface shape when manufactured. The lens reconstructs and enlarges a solar im ...
PDF only - at www.arxiv.org.
... (Non-coincident photoelectron pulses are monitored because there may be technical and economic reasons to use lesser peak power lasers with longer duration pulses. Alternatively the senders could use several even lower peak power lasers, operating at different wavelengths, and fired sequentially to ...
... (Non-coincident photoelectron pulses are monitored because there may be technical and economic reasons to use lesser peak power lasers with longer duration pulses. Alternatively the senders could use several even lower peak power lasers, operating at different wavelengths, and fired sequentially to ...
SPACE TELESCOPE SCIENCE INSTITUTE Bright Object Alerts
... Bright object alerts are reviewed by the Instrument Scientist during the normal proposal review. The submission of an approved review triggers flags in ASSIST to change the status of an alert from Pending to Waived. New alerts are generated every time NGSS is run. All alerts are stored in ASSIST unt ...
... Bright object alerts are reviewed by the Instrument Scientist during the normal proposal review. The submission of an approved review triggers flags in ASSIST to change the status of an alert from Pending to Waived. New alerts are generated every time NGSS is run. All alerts are stored in ASSIST unt ...
- River Bend Astronomy Club
... says of these automated eyes that “We probably operate about two-thirds of the nights that the weather is good and the moon is not bright. The telescopes, mounts and cameras have to be set and started before the run, which takes 15 or 20 minutes. It is possible to program unattended telescope runs l ...
... says of these automated eyes that “We probably operate about two-thirds of the nights that the weather is good and the moon is not bright. The telescopes, mounts and cameras have to be set and started before the run, which takes 15 or 20 minutes. It is possible to program unattended telescope runs l ...
Performance Improvement of a Flexible Telescope Through
... on a more realistic situation, the thermal and associated mechanical behavior of the telescope structure can be studied from thermal model calculations, which use as input a realistic thermal state of the environment [13]. The influence of wind on a telescope is investigated in a similar exploratory ...
... on a more realistic situation, the thermal and associated mechanical behavior of the telescope structure can be studied from thermal model calculations, which use as input a realistic thermal state of the environment [13]. The influence of wind on a telescope is investigated in a similar exploratory ...
sampling and characterization of the turbulence vertical distribution
... one of the Auxiliary Telescopes of the VLTI and will be used for the “site characterization” workpackage within of the ELT-FP6 project of the European Union. 3. STATISTICAL CRITERIA AND OBSERVATIONS In order to avoid biased statistical data, we have established to obtain the measurements in the peri ...
... one of the Auxiliary Telescopes of the VLTI and will be used for the “site characterization” workpackage within of the ELT-FP6 project of the European Union. 3. STATISTICAL CRITERIA AND OBSERVATIONS In order to avoid biased statistical data, we have established to obtain the measurements in the peri ...
PDF - Subaru Telescope
... IRD aims at detecting ~50 planets around nearby M dwarfs, including 10 Earth-like planets in habitable zone IRD will survey ~ 100 late M-dwarfs for 5 years and SSP is ...
... IRD aims at detecting ~50 planets around nearby M dwarfs, including 10 Earth-like planets in habitable zone IRD will survey ~ 100 late M-dwarfs for 5 years and SSP is ...
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.